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1. Determinants and treatments of heart failure after transcatheter aortic valve implantation: moving up a notch

Author

Kensuke Matsushita, Benjamin Marchandot, Antonin Trimaille, Sandy Hmadeh, Marion Kibler, Joe Heger, Adrien Carmona, Sebastien Hess, Antje Reydel, Laurence Jesel, Patrick Ohlmann, Valerie Schini‐Kerth, and Olivier Morel

Subjects
Transcatheter aortic valve implantation, Heart failure, Cardiac remodelling, Diseases of the circulatory (Cardiovascular) system, RC666-701
Abstract

Abstract Transcatheter aortic valve implantation (TAVI) has become an alternative to surgical aortic valve replacement for patients with symptomatic severe aortic stenosis in elderly and comorbid population. Significant improvement in heart function has been observed in patients undergoing TAVI, but numerous patients are readmitted to hospital for heart failure (HF). Moreover, repeat HF hospitalization is strongly associated with an adverse prognosis and increases the financial burden of health care. Although studies have identified pre‐existing and post‐procedural factors that contribute to HF hospitalization after TAVI, there is a paucity of data regarding optimal post‐procedural pharmacological treatments. This review aims to provide an overview of the current understanding of mechanisms, determinants, and potential treatments of HF following TAVI. We first review the pathophysiology of left ventricular (LV) remodelling, coronary microcirculation disorder, and endothelial dysfunction in patients with aortic stenosis and then examine the impact of TAVI on these conditions. We then present evidence of various factors and complications that may interplay with LV remodelling and contribute to HF events after TAVI. Next, we describe the triggers and predictors of early and late HF rehospitalizations following TAVI. Lastly, we discuss the potential of conventional pharmacological treatments, including renin–angiotensin blockers, beta‐blockers, and diuretics in TAVI patients. The paper explores the potential of newer drugs, including sodium–glucose co‐transporter 2 inhibitors, anti‐inflammatory drugs, and ion supplementation. Comprehensive knowledge in this field may aid in recognizing successful existing therapies, developing effective new treatments, and establishing dedicated patient care strategies during follow‐up after TAVI.

Published
2023
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2. Bitcoin and Its Energy, Environmental, and Social Impacts: An Assessment of Key Research Needs in the Mining Sector

Author

Murray A. Rudd, Lee Bratcher, Simon Collins, David Branscum, Matthew Carson, Shaun Connell, Elliot David, Magdalena Gronowska, Sebastien Hess, Austin Mitchell, Matt Prusak, Kyle Schneps, Maxim Serezhin, Scott A. Wolfe, and Dennis Porter

Subjects
bitcoin, bitcoin mining, energy transition, grid flexibility, key questions, research agenda, Technology, Science (General), Q1-390
Abstract

In this study, we used a combination of AI-assisted analysis of social media discourse and collaboration with industry experts to delve into the key research needs associated with the Bitcoin mining industry. We identified primary threats, opportunities, and research questions related to the Bitcoin mining industry and its wider impacts, focusing on its energy use and environmental footprint. Our findings spotlight the industry’s move towards increasingly greater energy efficiency and an emerging commitment to renewable energy, highlighting its potential to contribute to the coming energy transition. We underscore the transformative potential of emerging applications in the Bitcoin mining sector, especially regarding demand response, grid flexibility, and methane mitigation. We suggest that targeted research on Bitcoin can serve policymakers, private sector decision-makers, research funding agencies, environmental scientists, and the Bitcoin industry itself. We propose that filling key information gaps could help clarify the risks and benefits of Bitcoin mining by encouraging collaboration among researchers, policymakers, and industry stakeholders and conducting research that provides baseline peer-reviewed evidence surrounding Bitcoin’s production and impacts. A collaborative approach could help mitigate the risks and realize the benefits of Bitcoin mining, including potentially positive and substantive contributions in alignment with the Sustainable Development Goals.

Published
2023
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3. Increased susceptibility to SARS‐CoV‐2 infection in patients with reduced left ventricular ejection fraction

Author

Kensuke Matsushita, Benjamin Marchandot, Adrien Carmona, Anais Curtiaud, Anis El Idrissi, Antonin Trimaille, Marion Kibler, Thomas Cardi, Joe Heger, Sebastien Hess, Antje Reydel, Laurence Jesel, Patrick Ohlmann, and Olivier Morel

Subjects
Coronavirus disease 2019, Heart failure, Acute coronary syndrome, Diseases of the circulatory (Cardiovascular) system, RC666-701
Abstract

Abstract Aims Cardiovascular disease has been recognized as a major determinant of coronavirus disease 2019 (COVID‐19) vulnerability and severity. Angiotensin‐converting enzyme (ACE) 2 is a functional receptor for severe acute respiratory syndrome coronavirus 2 (SARS‐CoV‐2) and is up‐regulated in patients with heart failure. We sought to examine the potential association between reduced left ventricular ejection fraction (LVEF) and the susceptibility to SARS‐CoV‐2 infection. Methods and results Of the 1162 patients with acute coronary syndrome (ACS) who underwent percutaneous coronary intervention between February 2014 and October 2018, we enrolled 889 patients with available clinical follow‐up data. Follow‐up was conducted by telephone interviews 1 month after the start of the French lockdown which began on 17 March 2020. Patients were divided into two groups according to LVEF

Published
2021
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4. Acute kidney injury and acute kidney recovery following Transcatheter Aortic Valve Replacement

Author

Marilou Peillex, Benjamin Marchandot, Kensuke Matsushita, Eric Prinz, Sebastien Hess, Antje Reydel, Marion Kibler, Adrien Carmona, Antonin Trimaille, Joe Heger, Hélène Petit-Eisenmann, Annie Trinh, Laurence Jesel, Patrick Ohlmann, and Olivier Morel

Subjects
Medicine, Science
Abstract

Background Acute kidney injury (AKI) is associated with a dismal prognosis in Transcatheter Aortic Valve replacement (TAVR). Acute kidney recovery (AKR), a phenomenon reverse to AKI has recently been associated with better outcomes. Methods Between November 2012 to May 2018, we explored consecutive patients referred to our Heart Valve Center for TAVR. AKI was defined according to the VARC-2 definition. Mirroring the VARC-2 definition of AKI, AKR was defined as a decrease in serum creatinine (≥50%) or ≥25% improvement in GFR up to 72 hours after TAVR. Results AKI and AKR were respectively observed in 8.3 and 15.7% of the 574 patients included. AKI and AKR patients were associated to more advanced kidney disease at baseline. At a median follow-up of 608 days (range 355–893), AKI and AKR patients experienced an increased cardiovascular mortality compared to unchanged renal function patients (14.6% and 17.8% respectively, vs. 8.1%, CI 95%, pConclusions Both AKR and AKI negatively impact long term clinical outcomes of patients undergoing TAVR.

Published
2021

5. Effective Orifice Area of Balloon-Expandable and Self-Expandable Transcatheter Aortic Valve Prostheses: An Echo Doppler Comparative Study

Author

Mohamad Kanso, Marion Kibler, Sebastien Hess, Jérome Rischner, Philoktimon Plastaras, Michel Kindo, Minh Hoang, Fabien De Poli, Pierre Leddet, Hélène Petit, Floriane Zeyons, Annie Trinh, Kensuke Matsushita, Olivier Morel, and Patrick Ohlmann

Subjects
TAVI, Edwards Sapien 3, CoreValve, effective orifice area, transvalvular gradient, Doppler echocardiography, Medicine
Abstract

Published data on the size-specific effective orifice area (EOA) of transcatheter heart valves (THVs) remain scarce. Here, we sought to investigate the intra-individual changes in EOA and mean transvalvular aortic gradient (MG) of the Sapien 3 (S3), CoreValve (CV), and Evolut R (EVR) prostheses both at short-term and at 1-year follow-up. The study sample consisted of 260 consecutive patients with severe aortic stenosis who underwent transcatheter aortic valve implantation (TAVI). EOAs and MGs were measured with Doppler echocardiography for the following prostheses: S3 23 mm (n = 74; 28.5%), S3 26 mm (n = 67; 25.8%), S3 29 mm (n = 20; 7.7%), CV 23 mm (n = 2; 0.8%), CV 26 mm (n = 15; 5.8%), CV 29 mm (n = 24; 9.2%), CV 31 mm (n = 9; 3.5%), EVR 26 mm (n = 22; 8.5%), and EVR 29 mm (n = 27; 10.4%). Values were obtained at discharge, 1 month, 6 months, and 1 year from implantation. At discharge, EOAs were larger and MGs lower for larger-size prostheses, regardless of being balloon-expandable or self-expandable. In patients with small aortic annulus size, the hemodynamic performances of CV and EVR prostheses were superior to those of S3. However, we did not observe significant differences in terms of all-cause mortality according to THV type or size. Both balloon-expandable and self-expandable new-generation THVs show excellent hemodynamic performances without evidence of very early valve degeneration.

Published
2021
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9. Sun Planet Interactions Digital Environment on Request (SPIDER) for Europlanet RI H2024

Author

Anna Milillo, Sebastien Hess, Nicholas Achilleos, Patrick Guio, Yoshifumi Futaana, Baptiste Cecconi, Nicolas André, Andrea Opitz, Vincent Génot, and Alessandro Mura

Subjects
Spider, Geography, Planet, Astrobiology
Abstract

The H2020 Europlanet-2020 programme, which ended on Aug 31st, 2019, included an activity called PSWS (Planetary Space Weather Services), which provided 12 services distributed over four different domains (A. Prediction, B. Detection, C. Modelling, D. Alerts) and accessed through the PSWS portal (http://planetaryspaceweather-europlanet.irap.omp.eu/): A1. 1D MHD Solar Wind Prediction Tool – HELIOPROPA, A2. Propagation Tool, A3. Meteor showers, A4. Cometary tail crossings – TAILCATCHER, B1. Lunar impacts – ALFIE, B2. Giant planet fireballs – DeTeCt3.1, B3. Cometary tails – WINDSOCKS, C1. Earth, Mars, Venus, Jupiter coupling- TRANSPLANET, C2. Mars radiation environment – RADMAREE, C3. Giant planet magnetodiscs – MAGNETODISC, C4. Jupiter’s thermosphere, D. Alerts. In the framework of the starting Europlanet-2024 programme, SPIDER will extend PSWS domains (A. Prediction, C. Modelling, E. Databases) services and give the European planetary scientists, space agencies and industries access to 6 unique, publicly available and sophisticated services in order to model planetary environments and solar wind interactions through the deployment of a dedicated run on request infrastructure and associated databases. C5. A service for runs on request of models of Jupiter’s moon exospheres as well as the exosphere of Mercury, C6. A service to connect the open-source Spacecraft-Plasma Interaction Software (SPIS) software with models of space environments in order to compute the effect of spacecraft potential on scientific instruments onboard space missions. Pre-configured simulations will be made for Bepi-Colombo and JUICE missions, C7. A service for runs on request of particle tracing models in planetary magnetospheres, E1. A database of the high-energy particle flux proxy at Mars, Venus and comet 67P using background counts observed in the data obtained by the plasma instruments onboard Mars Express (operational from 2003), Venus Express (2006–2014), and Rosetta (2014–2015); E2. A simulation database for Mercury and Jupiter’s moons magnetospheres and link them with prediction of the solar wind parameters from Europlanet-RI H2020 PSWS services. A1. An extension of the Europlanet-RI H2020 PSWS Heliopropa service in order to ingest new observations from Solar missions like the ESA Solar Orbiter or NASA Solar Parker Probe missions and use them as input parameters for solar wind prediction; These developments will be discussed in the presentation. The Europlanet 2020 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 654208. The Europlanet 2024 Research Infrastructure project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.

Published
2020

10. DUSTER: a multi-sensor instrument to study dust transport and electrostatic removal for exploration missions

Author

Sebastien Hess, Johan De Keyser, Angel Alvaro Sanchez, Jean-Charles Mateo Velez, and Sylvain Ranvier

Subjects
business.industry, Environmental science, Aerospace engineering, business, Multi sensor
Abstract

One major environmental constraint during exploration missions is the presence of charged dust-like particles, which are present on the Moon, Mars, comets and asteroids. From an analysis of the effects of lunar dust on Extra-Vehicular Activity (EVA) systems during the six Apollo missions that landed on the lunar surface, it was found that these effects can take many forms such as external vision obscuration, false instrument readings, dust coating and contamination, loss of traction, clogging of mechanisms, abrasion, thermal control problems and seal failures. One of the most serious effects is the compromising of astronaut health by irritation and inhalation of lunar dust.Therefore, it is of utmost importance to characterise the properties of the dust particles present on the exploration sites and their transportation mechanisms to enable efficient mitigation techniques to be put in place.The overall objective of the DUSTER project is to develop instrumentation and technologies to study dust particles and electrostatic transportation for planetary and small body exploration missions. Specifically, the aim is to design, manufacture and test in a relevant environment a compact multi-sensor instrument for in situ analysis of dust properties (mechanical and electrical) and electrostatic transportation that can be used on a small lunar lander. To that end, the instrument includes:- A dust collector: electrodes biased at high potential to attract/collect dust particles, coupled to an electrometer- Langmuir probes- E-field probesUsing this instrument, the following parameters will be derived:- Charging level of dust as a function of the environmental parameters (illumination, plasma density and temperature)- (gravity + cohesive forces)/charge ratio distribution of dust layerThese two parameters will allow the determination of the electric field needed to attract/collect dust according to the environmental conditions (illumination, plasma density and temperature), which, among other applications, will allow designing electrostatic dust mitigation devices and dust sample collectors.

Published
2020

11. Reply to comment 'On the hydrogen escape: Comment to variability of the hydrogen in the Martian upper atmosphere as simulated by a 3D atmosphere-exosphere coupling by J.-Y. Chaufray et al.' by V. Krasnopolsky, Icarus, 281, 262

Author

Ronan Modolo, Francisco Gonzalez-Galindo, Jean-Yves Chaufray, François Forget, Miguel Lopez-Valverde, François Leblanc, Sebastien Hess, European Commission, Centre National de la Recherche Scientifique (France), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), HELIOS - LATMOS, ONERA - The French Aerospace Lab [Toulouse], ONERA, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL)

Subjects
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Martian, Physics, 010504 meteorology & atmospheric sciences, Atmospheric escape, Hydrogen, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Flux, chemistry.chemical_element, Astronomy and Astrophysics, Mars Exploration Program, Atmospheric sciences, 01 natural sciences, Atmosphere, Solar wind, chemistry, 13. Climate action, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Exosphere
Abstract

Krasnopolsky (2017) makes a careful review of our recent results about the Martian hydrogen content of the Martian upper atmosphere (Chaufray et al., 2015). We comment here on his two major points. First, he suggests that the non-thermal escape of H, and particularly collisions with hot oxygen, not taken into account in our general circulation model (GCM), should modify our reported H and H density profiles. This is an important issue; we acknowledge that future effective coupling of our GCM with comprehensive models of the Martian solar wind interaction, ideally after being validated with the latest plasma observations of H , would allow for better estimations of the relative importance of the H non-thermal and thermal escape processes. For the time being we need assumptions in the GCM, with proper and regular updates. According to a recent and detailed study of the anisotropic elastic and inelastic collision cross sections between O and H (Gacesa et al., 2012), the escape rates used by Krasnopolsky (2010) for this process might be overestimated. We therefore do not include non thermal escape of H in the model. And secondly, in response to Krasnopolsky's comment on the H escape variability with the solar cycle, we revised our calculations and found a small bug in the computation of the Jeans effusion velocity. Our revised computed H escape rates are included here. They have a small impact on our key conclusions: similar seasonal variations, a reduced variation with the solar cycle but still larger than Krasnopolsky (2017), and again a hydrogen scape systematically lower than the diffusion-limited flux. This bug does not affect the latest Mars Climate Database v5.2. © 2017 Elsevier Inc., This work has been partially funded by the European Union Horizon 2020 Programme (H2020 Compet -08-2014) under grant agreement UPWARDS-633127. We thank Programme National de Planetologie (PNP) and Programme National Soleil-Terre (PNST) for their support.

Published
2018

12. Detection of Jupiter decametric emissions controlled by Europa and Ganymede with Voyager/PRA and Cassini/RPWS

Author

Baptiste Cecconi, Laurent Lamy, Corentin Louis, Sebastien Hess, and Philippe Zarka

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Jovian, Physics::Geophysics, Astrobiology, Jupiter, symbols.namesake, Exploration of Jupiter, 0103 physical sciences, Statistical analysis, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Astronomy, Galilean moons, Geophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, symbols, Environmental science, Astrophysics::Earth and Planetary Astrophysics, Longitude
Abstract

The Jovian high-latitude radio emissions produced by Jupiter's magnetosphere extend from a few kilohertz to 40 MHz. Part of the decametric (DAM) emissions are driven by the Galilean moon Io (Io-DAM). As UV aurorae have been detected at the footprint of Europa and Ganymede, we expect that these moons drive Jovian radio emissions as well. To check this assumption, we used the ExPRES simulation code (Exoplanetary and Planetary Radio Emissions Simulator) to predict dynamic spectrum (time-frequency spectograms) of the radio emissions controlled by the four Galilean moons. Then we compared the simulations to the Voyager/PRA and Cassini/RPWS radio observations of Jupiter (1979, and between 2000 and 2003, respectively). We present the first clear evidence for the existence of decametric emissions controlled by Europa and Ganymede. Their statistical analysis allows us to describe the average properties of the Europa-DAM and Ganymede-DAM emissions such as their spectrum, temporal variability, and occurrence as a function of moon phase and subobserver's longitude.

Published
2017

13. ExPRES: an Exoplanetary and Planetary Radio Emissions Simulator

Author

Stéphane Aicardi, Baptiste Cecconi, Corentin Louis, Sebastien Hess, A. Loh, Laurent Lamy, P. Zarka, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Direction Informatique de l'Observatoire - Composante PADC (DIO - PADC), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), and PRES Université de Toulouse-ONERA

Subjects
Rotation period, Outer planets, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Instability, law.invention, Acceleration, [SPI]Engineering Sciences [physics], law, 0103 physical sciences, Maser, 010303 astronomy & astrophysics, Simulation, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Computer Science::Information Retrieval, Astronomy and Astrophysics, Orbital period, Exoplanet, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context. Earth and outer planets are known to produce intense non-thermal radio emissions through a mechanism known as cyclotron maser instability (CMI), requiring the presence of accelerated electrons generally arising from magnetospheric current systems. In return, radio emissions are a good probe of these current systems and acceleration processes. The CMI generates highly anisotropic emissions and leads to important visibility effects, which have to be taken into account when interpreting the data. Several studies have shown that modelling the radio source anisotropic beaming pattern can reveal a wealth of physical information about the planetary or exoplanetary magnetospheres that produce these emissions. Aims. We present a numerical tool, called ExPRES (Exoplanetary and Planetary Radio Emission Simulator), which is able to reproduce the occurrence in a time-frequency plane of R−X CMI-generated radio emissions from planetary magnetospheres, exoplanets, or star–planet interacting systems. Special attention is given to the computation of the radio emission beaming at and near its source. Methods. We explain what physical information about the system can be drawn from such radio observations, and how it is obtained. This information may include the location and dynamics of the radio sources, the type of current system leading to electron acceleration and their energy, and, for exoplanetary systems, the orbital period of the emitting body and the strength, rotation period, tilt, and the offset of the planetary magnetic field. Most of these parameters can only be remotely measured via radio observations. Results. The ExPRES code provides the proper framework of analysis and interpretation for past, current, and future observations of planetary radio emissions, as well as for future detection of radio emissions from exoplanetary systems (or magnetic, white dwarf–planet or white dwarf–brown dwarf systems). Our methodology can be easily adapted to simulate specific observations once effective detection is achieved.

Published
2019

14. P2Y

Author

Kensuke, Matsushita, Benjamin, Marchandot, Marion, Kibler, Antonin, Trimaille, Sebastien, Hess, Lelia, Grunebaum, Antje, Reydel, Laurence, Jesel, Patrick, Ohlmann, and Olivier, Morel

Subjects
Transcatheter Aortic Valve Replacement, Purinergic P2Y Receptor Antagonists, Humans, Postoperative Hemorrhage, Clopidogrel
Published
2019

15. Detecting exoplanets with FAST?

Author

P. Zarka, Jean-Mathias Grießmeier, T. Joseph W. Lazio, Sebastien Hess, Gregg Hallinan, Laurent Lamy, Di Li, Julien N. Girard, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), National Astronomical Observatory, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, ONERA - The French Aerospace Lab [Toulouse], ONERA, California Institute of Technology (CALTECH), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
radio continuum: planetary systems, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, telescopes (radio), Physical information, 0103 physical sciences, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy and Astrophysics, radiation mechanisms: non-thermal, plasmas, Exoplanet, planets and satellites: magnetic fields, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, methods: observational, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We briefly review the various proposed scenarios that may lead to nonthermal radio emissions from exoplanetary systems (planetary magnetospheres, magnetosphere-ionosphere and magnetosphere-satellite coupling, and star-planet interactions), and the physical information that can be drawn from their detection. The latter scenario is especially favorable to the production of radio emission above 70\,MHz. We summarize the results of past and recent radio searches, and then discuss FAST characteristics and observation strategy, including synergies. We emphasize the importance of polarization measurements and a high duty-cycle for the very weak targets that radio-exoplanets prove to be., 6 pages, 3 figures, published in the mini-volume on FAST science potentials in the journal Research in Astronomy and Astrophysics

Published
2019

16. The SPASE Data Model: A Metadata Standard for Registering, Finding, Accessing, and Using Heliophysics Data Obtained from Observations and Modeling

Author

D. L. De Zeeuw, Vincent Génot, Sebastien Hess, Baptiste Cecconi, James R. Thieman, D. Aaron Roberts, Chiu Wiegand, Shing F. Fung, Todd King, Chris Perry, Michel Gangloff, NASA Goddard Space Flight Center (GSFC), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Atmospheric Science, Information retrieval, 010504 meteorology & atmospheric sciences, Application programming interface, Computer science, Metadata standard, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], computer.software_genre, 01 natural sciences, Backward compatibility, Identifier, Data access, Heliophysics, Data model, 0103 physical sciences, Web service, 010303 astronomy & astrophysics, computer, 0105 earth and related environmental sciences
Abstract

The Space Physics Archive Search and Extract Consortium has developed and implemented the SPASE Data Model that provides a common language for registering a wide range of Heliophysics data and other products. The Data Model enables discovery and access tools such that any researcher can obtain data easily, thereby facilitating research, including on space weather. The Data Model includes descriptions of Simulation Models and Numerical Output, pioneered by the Integrated Medium for Planetary Exploration (IMPEx) group in Europe, and subsequently adopted by the Community Coordinated Modeling Center (CCMC). The SPASE group intends to register all relevant Heliophysics data resources, including space-, ground-, and model-based. Substantial progress has been made, especially for space-based observational data and associated observatories, instruments, and display data. Legacy product registrations and access go back more than 50 years. Real-time data will be included. The National Aeronautics and Space Administration (NASA) portion of the SPASE group has funding that assures continuity in the upkeep of the Data Model and aids with adding new products. Tools are being developed for making and editing data descriptions. Digital Object Identifiers (DOIs) for Data Products can now be included in the descriptions. The data access that SPASE facilitates is becoming more uniform, and work is progressing on Web Service access via a standard Application Programming Interface. The SPASE Data Model is stable; changes over the past 9 years were additions of terms and capabilities that are backward compatible. This paper provides a summary of the history, structure, use, and future of the SPASE Data Model.

Published
2018

17. Mars-solar wind interaction: LatHyS, an improved parallel 3-D multispecies hybrid model

Author

François Forget, Francisco Gonzalez-Galindo, David Brain, Rosa Esteban-Hernandez, Christian Mazelle, François Leblanc, Marco Mancini, Manabu Yagi, Jean-Yves Chaufray, Ronan Modolo, Sebastien Hess, Ludivine Leclercq, Gérard Chanteur, and Philippe Weill

Subjects
Martian, Physics, 010504 meteorology & atmospheric sciences, Magnetosphere, Scale height, Mars Exploration Program, Geophysics, 01 natural sciences, Corona, Computational physics, Solar wind, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Ionosphere, 010303 astronomy & astrophysics, Image resolution, 0105 earth and related environmental sciences
Abstract

In order to better represent Mars-Solar wind interaction, we present an unprecedented model achieving spatial resolution down to 50 km, a so far unexplored resolution for global kinetic models of the Martian ionized environment. Such resolution approaches the ionospheric plasma scale height. In practice, the model is derived from a first version described in Modolo et al. [2005]. An important effort of parallelization has been conducted and is presented here. A better description of the ionosphere was also implemented including ionospheric chemistry, electrical conductivities and a drag force modelling the ion-neutral collisions in the ionosphere. This new version of the code, named LatHyS (Latmos Hybrid Simulation), is here used to characterize the impact of various spatial resolutions on simulation results. In addition, and following a global model challenge effort [Brain et al., 2010], we present the results of simulation run for three cases which allows addressing the effect of the supra-thermal corona and of the solar EUV activity on the magnetospheric plasma boundaries and on the global escape. Simulation results showed that global patterns are relatively similar for the different spatial resolution runs but finest grid runs provide a better representation of the ionosphere and display more details of the planetary plasma dynamic. Simulation results suggest that a significant fraction of escaping O+ ions is originated from below 1200 km altitude.

Published
2016

18. Lunar dust simulant charging and transport under UV irradiation in vacuum: Experiments and numerical modeling

Author

A. Champlain, P. Sarrailh, G. Murat, J.-P. Chardon, J. F. Roussel, A. Gajan, Sebastien Hess, and J.-C. Matéo-Vélez

Subjects
Physics, Geophysics, 010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, Numerical modeling, Irradiation, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences, Astrobiology
Published
2016

19. Simulating Jupiter-satellite decametric emissions with ExPRES: A parametric study

Author

Xavier Bonnin, Sebastien Hess, Ph. Zarka, Corentin Louis, Laurent Lamy, and Baptiste Cecconi

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, FOS: Physical sciences, Magnetosphere, Physics::Geophysics, Computational physics, Magnetic field, law.invention, Jupiter, law, Physics::Space Physics, Satellite, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Maser, Astrophysics - Earth and Planetary Astrophysics, Parametric statistics
Abstract

The high latitude radio emissions produced by the Cyclotron Maser Instability (CMI) in Jupiter's magnetosphere extend from a few kHz to 40 MHz. Part of the decametric emissions is of auroral origin, and part is driven by the moons Io, Europa and Ganymede. After summarizing the method used to identify Jupiter-satellite radio emissions, which consists in comparing space- and ground-based radio observations to ExPRES simulations of CMI-driven emissions in the time-frequency plane, we present a parametric study of the free parameters required by the ExPRES code (electron distribution function and resonant energy, magnetic field model, lead angle, and altitude of the ionospheric cut-off) in order to assess the accuracy of our simulations in the Io-Jupiter case. We find that Io-DAM arcs are fairly modeled by loss-cone driven CMI with electrons of 1-10 keV energy, using the ISaAC, VIPAL or VIP4 magnetic field model and a simple sinusoidal lead angle model. The altitude of the ionospheric cut-off has a marginal impact on the simulations. We discuss the impact of our results on the identification of Europa-DAM and Ganymede-DAM emissions., 14 pages, 2 figures, Planetary Radio Emissions VIII

Published
2018

20. Effects of the Crustal Magnetic Fields and Changes in the IMF Orientation on the Magnetosphere of Mars: MAVEN Observations and LatHyS Results

Author

Sebastien Hess, David Brain, Jean-Yves Chaufray, Bruce M. Jakosky, Ronan Modolo, James P. McFadden, François Leblanc, Norberto Romanelli, John E. P. Connerney, Jasper Halekas, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), ONERA / DPHY, Université de Toulouse [Toulouse], ONERA-PRES Université de Toulouse, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), ANR-17-CE31-0016,TEMPETE,Évolutions temporelles des environnements planétaires magnétisés pendant des tempêtes solaires(2017), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of California [Berkeley], University of California-University of California, HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), ONERA - The French Aerospace Lab ( Toulouse ), ONERA, Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], NASA Goddard Space Flight Center ( GSFC ), University of Iowa [Iowa], and Space Sciences Laboratory [Berkeley] ( SSL )

Subjects
010504 meteorology & atmospheric sciences, CRUSTAL MAGNETIC FIELD EFFECT, Magnetosphere, Astrophysics, 01 natural sciences, IMF ORIENTATION, MARTIAN MAGNETOSPHERE, 0103 physical sciences, Interplanetary magnetic field, 010303 astronomy & astrophysics, O+ ION LOSS RATE, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], 0105 earth and related environmental sciences, RECOVERY TIMESCALE, Martian, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], MARS, Plasma, Atmosphere of Mars, Mars Exploration Program, H+ ION LOSS RATE, Magnetic field, Solar wind, Geophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics
Abstract

International audience; The Mars Atmosphere and Volatile EvolutioN Mission (MAVEN) is currently probing the complex Martian environment. Although main structures arising from the interaction between the solar wind (SW) and the induced magnetosphere of Mars can be described using a steady state picture, time‐dependent physical processes modify the response of this obstacle. These processes result from temporal variabilities in the internal and/or external electromagnetic fields and plasma properties. Indeed, the crustal magnetic fields (CF) rotation constantly modifies the intrinsic magnetic field topology relative to the SW. Moreover, the magnetosphere's state is also modified by changes in the interplanetary magnetic field (IMF). In this work we analyze MAVEN magnetic field and plasma measurements obtained on 23 December 2014, between 06:00 UT ‐ 14:15 UT. These measurements suggest the external conditions remained approximately constant when MAVEN was inside the magnetosphere during the first orbit. In contrast, MAVEN observed changes in the IMF orientation before visiting the magnetosphere during the second orbit. To investigate the response of the Martian plasma environment to the CF rotation and IMF variability, we also perform hybrid simulations, using MAVEN observations to set SW external conditions. Simulation results are compared with the MAVEN measurements and show good agreement. Associated recovery timescales of different magnetospheric regions are found to range between ∼ 10 s and ∼ 10 min. Finally, we do not observe large variability in the total planetary H+ and O+ escape rates at different times during this event, although a correlation between the latter and the CFs location is identified.

Published
2018

21. Science data visualization in planetary and heliospheric contexts with 3DView

Author

Alexis P. Rouillard, Christian Jacquey, Nicolas André, Maxim L. Khodachenko, M. Bouchemit, Vincent Génot, Elena Budnik, S. Caussarieu, N. Jourdane, Manuel Scherf, Fédéric Pitout, Baptiste Cecconi, Rui Pinto, Stéphane Erard, Ronan Modolo, T. Al-Ubaidi, J.-P. Toniutti, Joelle Durand, D. Popescu, Michel Gangloff, Ludivine Leclercq, L. Beigbeder, Sebastien Hess, N. Dufourg, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), GFI Informatique, Centre National d'Études Spatiales [Toulouse] (CNES), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), ONERA - The French Aerospace Lab [Toulouse], ONERA, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), D.V. Skobeltsyn Institute of Nuclear Physics (SINP), Lomonosov Moscow State University (MSU), European Union, CNES, European Project: 262863,EC:FP7:SPA,FP7-SPACE-2010-1,IMPEX(2011), European Project: 654208,H2020,H2020-INFRAIA-2014-2015,EPN2020-RI(2015), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), HEPPI - LATMOS, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, 010504 meteorology & atmospheric sciences, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Space physics, External Data Representation, 01 natural sciences, Rendering (computer graphics), Upload, Data visualization, Software, Heliophysics, Space and Planetary Science, Human–computer interaction, 0103 physical sciences, Data center, business, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; We present a 3D orbit viewer application capable of displaying science data. 3DView, a web tool designed by the French Plasma Physics Data Centre (CDPP) for the planetology and heliophysics community, has extended functionalities to render space physics data (observations and models alike) in their original 3D context. Time series, vectors, dynamic spectra, celestial body maps, magnetic field or flow lines, 2D cuts in simulation cubes, etc, are among the variety of data representation enabled by 3DView. The direct connection to several large databases, the use of VO standards and the possibility to upload user data makes 3DView a versatile tool able to cover a wide range of space physics contexts. The code is open source and the software is regularly used at Masters Degree level or summer school for pedagogical purposes. The present paper describes the general architecture and all major functionalities, and offers several science cases (simulation rendering, mission preparation, etc.) which can be easily replayed by the interested readers. Future developments are finally outlined.

Published
2018
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22. The LatHyS database for planetary plasma environment investigations: Overview and a case study of data/model comparisons

Author

David Brain, Maxim L. Khodachenko, Bruce M. Jakosky, Shannon Curry, Morgane Steckiewicz, J.-P. Toniutti, E. Budnik, L. Beigbeder, Vincent Génot, François Leblanc, Mats Holmström, Nicolas André, Andrei Fedorov, Ronan Modolo, T. Al-Ubaidi, Jean-Yves Chaufray, Sebastien Hess, Philippe Weill, M. Bouchemit, Michel Gangloff, D. Popescu, Ludivine Leclercq, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), ONERA - The French Aerospace Lab [Toulouse], ONERA, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Department of Materials Science and Engineering [Charlottesville] (MS), University of Virginia [Charlottesville], Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), NOVELTIS [Sté], GFI Informatique, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Swedish Institute of Space Physics [Kiruna] (IRF), European Union, Agence Nationale de la Recherche (ANR), ANR-09-BLAN-0223,HELIOSARES,Relation Soleil ? Mars: description et analyse des échanges présents et passés entre magnétosphère et atmosphère(2009), ANR-13-BS05-0012,MARMITE,Mercure: interActions HeRméo-Magnétiques entre l'InTérieur et l'Exosphère(2013), European Project: 262863,EC:FP7:SPA,FP7-SPACE-2010-1,IMPEX(2011), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Virginia, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)

Subjects
010504 meteorology & atmospheric sciences, Computer science, Data management, Interoperability, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Numercial modeling, computer.software_genre, 01 natural sciences, Solar wind interactions with unmagnetized bodies, 0103 physical sciences, Representation (mathematics), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Martian, Database, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Mars Exploration Program, Planetary plasma, Solar wind, Data model, 13. Climate action, Space and Planetary Science, Web service, business, computer, LatHyS database
Abstract

International audience; We present the Latmos Hybrid Simulation (LatHyS) database, which is dedicated to the investigations of planetary plasma environment. Simulation results of several planetary objects (Mars, Mercury, Ganymede) are available in an online catalogue. The full description of the simulations and their results is compliant with a data model developped in the framework of the FP7 IMPEx project. The catalogue is interfaced with VO-visualization tools such AMDA, 3DView, TOPCAT, CLweb or the IMPEx portal. Web services ensure the possibilities of accessing and extracting simulated quantities/data. We illustrate the interoperability between the simulation database and VO-tools using a detailed science case that focuses on a three-dimensional representation of the solar wind interaction with the Martian upper atmosphere, combining MAVEN and Mars Express observations and simulation results.

Published
2018

23. SPIS 5: New Modeling Capabilities and Methods for Scientific Missions

Author

B. Thiebault, D. Rodgers, Pierre Sarrailh, Denis Payan, Alain Hilgers, Sebastien Hess, Fabrice Cipriani, Julien Forest, Benjamin Jeanty-Ruard, Jean-Charles Mateo-Velez, and Jean-François Roussel

Subjects
Physics, Nuclear and High Energy Physics, User Friendly, Spacecraft, business.industry, Photovoltaic system, Detector, Electrical engineering, Condensed Matter Physics, symbols.namesake, Software, Physics::Space Physics, symbols, Langmuir probe, Aerospace engineering, User interface, business, Spinning
Abstract

Since the last version, the numerical core and the user interface of Spacecraft Plasma Interaction Software (SPIS) have been significantly improved to achieve two objectives: 1) to make SPIS more user friendly and robust for industrial use and 2) to extend the multiscale capabilities and the precision of the solvers in order to model a large range of scientific missions. The new numerical algorithm and modeling capabilities are presented in detail. This new version permits modeling of time variations of the plasma environment, spinning spacecraft, semitransparent grids, secondary emission from 1-D thin elements (e.g., wires or booms), 2-D thin elements (for example, solar arrays), the effect of $v\times B$ electric field, particle detectors, and Langmuir probes onboard spacecraft.

Published
2015

24. Refurbishing Voyager 1 & 2 Planetary Radio Astronomy (PRA) Data

Author

D. R. Evans, Corentin Louis, Danièle Boucon, Laurent Lamy, Baptiste Cecconi, Sebastien Hess, Anaïs Pruvot, Philippe Zarka, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris

Subjects
Jupiter, Earth and Planetary Astrophysics (astro-ph.EP), Saturn, Astronomy, FOS: Physical sciences, Great conjunction, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Data calibration, Geology, Radio astronomy, Astrophysics - Earth and Planetary Astrophysics
Abstract

Voyager/PRA (Planetary Radio Astronomy) data from digitized tapes archived at CNES have been reprocessed and recalibrated. The data cover the Jupiter and Saturn flybys of both Voyager probes. We have also reconstructed goniopolarimetric datasets (flux and polarization) at full resolution. These datasets are currently not available to the scientific community, but they are of primary interest for the analysis of the Cassini data at Saturn, and the Juno data at Jupiter, as well as for the preparation of the JUICE mission. We present the first results derived from the re-analysis of this dataset., Comment: Accepted manuscript for PRE8 (Planetary Radio Emission VIII conference) proceedings

Published
2017
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25. Io-Jupiter decametric arcs observed by Juno/Waves compared to ExPRES simulations

Author

Steven Levin, Scott Bolton, George Hospodarsky, Corentin Louis, William S. Kurth, Masafumi Imai, John E. P. Connerney, Sebastien Hess, Baptiste Cecconi, Ph. Zarka, Laurent Lamy, X. Bonnin, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), University of Iowa [Iowa City], Department of Physics and Astronomy [Iowa City], ONERA - The French Aerospace Lab [Toulouse], ONERA, Southwest Research Institute [San Antonio] (SwRI), NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), and California Institute of Technology (CALTECH)-NASA

Subjects
Physics, 010504 meteorology & atmospheric sciences, Plane (geometry), Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Astronomy, 01 natural sciences, Instability, Latitude, law.invention, Galilean moons, Jupiter, symbols.namesake, Geophysics, law, 0103 physical sciences, Physics::Space Physics, symbols, General Earth and Planetary Sciences, Maser, Decametre, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; We compare observations from the Juno/Waves radio experiment with simulations of radio «arcs» in the time-frequency plane resulting from the Io-Jupiter interaction, performed with the ExPRES code. We identify the hemisphere of origin of the observed arcs directly from simulations and confirm this identification through comparison with Juno, Nançay, and Wind observations. The occurrence and shape of observed arcs are well modeled, at low latitudes with their usual shapes as seen from Earth, as well as at high latitudes with longer, bowl-shaped, arcs observed for the first time. Predicted emission is actually observed only when the radio beaming angle θ = (k,B) ≥ 70° ± 5°, providing new constraints on the generation of the decameter emission by the Cyclotron Maser Instability. Further improvements of ExPRES are outlined, which will then be applied to Juno and Earth-based observations of radio emissions induced by other Galilean satellites or associated to the main auroral oval.

Published
2017

26. A Study of Solar Orbiter Spacecraft–Plasma Interactions Effects on Electric Field and Particle Measurements

Author

Stanislas Guillemant, Jean-Charles Mateo-Velez, Filippo Pantellini, Christopher J. Owen, Sebastien Hess, Antonio Vecchio, Pierre Sarrailh, Vincent Génot, Laurent Lamy, Milan Maksimovic, Alain Hilgers, Philippe Louarn, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), MSSL, UCL, stfc, ONERA - The French Aerospace Lab [Toulouse], ONERA, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and European Space Agency (ESA)

Subjects
ASTROPHYSICS, Nuclear and High Energy Physics, ELECTROSTATIC MEASUREMENTS, 010504 meteorology & atmospheric sciences, ELECTRIC POTENTIAL, Electron, PLASMA SIMULATION, 7. Clean energy, 01 natural sciences, Electromagnetic radiation, Space exploration, 010305 fluids & plasmas, law.invention, ARTIFICIAL SATELLITES, Orbiter, SPACE EXPLORATION, law, Physics::Plasma Physics, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], 0103 physical sciences, Thermal, Astrophysics::Solar and Stellar Astrophysics, Aerospace engineering, 0105 earth and related environmental sciences, Remote sensing, Physics, Spacecraft, business.industry, Plasma, Condensed Matter Physics, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Solar wind, 13. Climate action, AEROSPACE SIMULATION, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, PLASMA MEASUREMENTS
Abstract

International audience; We present numerical simulations of the Solar Orbiter spacecraft (SC)/plasma interaction performed with the SC–plasma interaction system software. Solar orbiter, to be launched in 2019, is dedicated to observe the sun and the solar wind. The SC will be equipped with both in situ and remote sensing instruments and will approach the sun as close as 0.28 AU. The whole SC will be subjected to an intense electromagnetic radiation flux (ten times that at the earth) leading to specific thermal and SC–plasma interactions issues. This paper investigates plasma interaction effects with two instruments: the radio and plasma waves and the electron analyzer system.

Published
2017

27. Three-dimensional Martian ionosphere model: I. The photochemical ionosphere below 180 km

Author

Sebastien Hess, François Leblanc, Francisco Gonzalez-Galindo, Jean-Yves Chaufray, Gabriella Gilli, M. Yagi, Ronan Modolo, François Forget, and Miguel Lopez-Valverde

Subjects
Martian, 010504 meteorology & atmospheric sciences, Solar zenith angle, Mars Exploration Program, Geophysics, Atmospheric sciences, Photochemistry, 01 natural sciences, Physics::Geophysics, Solar cycle, Mars general circulation model, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Physics::Space Physics, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Solar rotation, Timekeeping on Mars, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

[1] We describe the Mars ionosphere with unprecedented detail in 3-D, as simulated by a Mars general circulation model (the Laboratoire de Meteorologie Dynamique Mars GCM), and compare it with recent measurements. The model includes a number of recent extensions and improvements. Different simulations for a full Martian year have been performed. The electron density at the main ionospheric peak is shown to vary with the Sun-Mars distance and with the solar variability, both in the long-term (11 year solar cycle) and on shorter temporal scales (solar rotation). The main electronic peak is shown to be located at the same pressure level during all the Martian year. As a consequence, its altitude varies with latitude, local time, and season according to the natural expansions and fluctuations of the neutral atmosphere, in agreement with previous models. The model predicts a nighttime ionosphere due only to photochemistry. The simulated ionosphere close to the evening terminator is in agreement with observations. No effort has been made to explain the patchy ionosphere observed in the deep nightside. We have compared the modeled ionosphere with Mars Global Surveyor and Mars Advanced Radar for Subsurface and Ionosphere Sounding data. The model reproduces the solar zenith angle variability of the electron density and the altitude of the peak, although it underestimates the electron density at the main peak by about 20%. The electron density at the secondary peak is strongly underestimated by the model, probably due to a very crude representation of the X-ray solar flux. This is one of the aspects that needs a revision in future versions of the model.

Published
2013

28. Combination of Primary Hemostatic Disorders and Atrial Fibrillation Increases Bleeding Events Following Transcatheter Aortic Valve Replacement

Author

Kensuke Matsushita, Benjamin Marchandot, Marion Kibler, Adrien Carmona, Truong Dinh Phi, Joe Heger, Antonin Trimaille, Sébastien Hess, Laurent Sattler, Mickael Ohana, Antje Reydel, Laurence Jesel, Patrick Ohlmann, and Olivier Morel

Subjects
transcatheter aortic valve replacement, atrial fibrillation, closure time of adenosine diphosphate, primary hemostasis, bleeding events, Diseases of the circulatory (Cardiovascular) system, RC666-701
Abstract

Background Patients with atrial fibrillation (AF) are likely to have a poor prognosis including bleedings following transcatheter aortic valve replacement (TAVR). Closure time of adenosine diphosphate (CT-ADP) is a primary hemostasis point-of-care test and is a predictor of bleeding events following TAVR. We aimed to evaluate the impact of ongoing primary hemostatic disorders on bleeding events in TAVR patients with AF. Methods We enrolled 878 patients from our prospective registry. The primary endpoint was VARC-2 major/life-threatening bleeding complications (MLBCs) at 1 year after TAVR and secondary endpoint was major adverse cardiac and cerebrovascular events (MACCEs) at 1 year, defined as a composite of all-cause death, myocardial infarction, stroke, and heart failure hospitalization. Ongoing primary hemostatic disorder was defined by a postprocedural CT-ADP >180 seconds. Results Patients with AF had a higher incidence of MLBCs (20 vs. 12%, p = 0.002), MACCE (29 vs. 20%, p = 0.002), and all-cause mortality (15 vs. 8%, p = 0.002) within 1 year compared to non-AF patients. When the cohort was split into four subgroups according to AF and CT-ADP >180 seconds, patients with AF and CT-ADP >180 seconds had the highest risk of MLBCs and MACCE. Multivariate Cox regression analysis confirmed that the patients with AF and CT-ADP >180 seconds had 3.9-fold higher risk of MLBCs, whereas those patients were no longer associated with MACCE after the adjustment. Conclusion In TAVR patients, AF with postprocedural CT-ADP >180 seconds was strongly associated with MLBCs following TAVR. Our study suggests that persistent primary hemostatic disorders contribute to a higher risk of bleeding events particularly in AF patients.

Published
2023
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29. Mars exospheric thermal and non-thermal components: Seasonal and local variations

Author

Ronan Modolo, Francisco Gonzalez-Galindo, Manabu Yagi, Sebastien Hess, Jean-Yves Chaufray, François Leblanc, Solar-Terrestrial Environment Laboratory [Nagoya] (STEL), Nagoya University, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Flux, chemistry.chemical_element, Atmospheric sciences, 7. Clean energy, 01 natural sciences, Oxygen, Planet, Atmospheric Evolution, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Martian, Astronomy and Astrophysics, Scale height, Atmosphere of Mars, Mars Exploration Program, chemistry, 13. Climate action, Space and Planetary Science, Simulation, Exosphere
Abstract

A model of the martian exosphere is built for average solar conditions. A Chamberlain’s approach (Chamberlain, J.W. [1963]. Planet. Space Sci. 11, 901) is used to describe the O, CO, CO 2 , and O 2 thermal exospheric components. The average thermal oxygen density at 300 km in altitude varies by about one order of magnitude with seasons. A Monte-Carlo test particle simulation is also developed in order to estimate the non-thermal oxygen component of the exosphere. The seasonal variation of the non-thermal oxygen average density is much less than the thermal component but displays clear seasonal variations of its spatial distribution. The neutral oxygen atomic escaping flux varies from 2.9 to 5.3 × 10 25 s −1 in good agreement with Valeille et al. (Valeille, A., Combi, M.R., Bougher, S.W., Tenishev, V., Nagy, A.F. [2009a]. J. Geophys. Res. (Planets) 114, 11006; Valeille, A., Tenishev, V., Bougher, S.W., Combi, M.R., Nagy, A.F. [2009b]. J. Geophys. Res. (Planets) 114, 11005). Mars’s oxygen exosphere is thermal below 600 km and non-thermal above 700 km at all seasons. The typical scale height is ∼45 km for thermal O and ∼500 km for the non-thermal oxygen density. The total photoionization rate above 300 km corresponds to a CO 2 + / O + total production ratio between 0.004 and 0.02. When compared to the composition of the escaping flux measured by ASPERA-3/Mars Express, this suggests that ions formed below 300 km should significantly contribute to the escaping ion flux and/or that a significant part of the newly O + ions reimpacts Mars. The simulated oxygen density profile is also compared to the recent observed profile by Alice/Rosetta (Feldman, P.D. et al. [2011]. Icarus 214, 394–399). Although the scale height of our simulated non-thermal oxygen exosphere and the transition from thermal to non-thermal dominated exospheres are slightly higher than suggested by Feldman et al. (Feldman, P.D. et al. [2011]. Icarus 214, 394–399), a good agreement is found when taking into account the uncertainties of Alice/Rosetta observations.

Published
2012

30. Imaging Jupiter's radiation belts down to 127 MHz with LOFAR

Author

Gianni Bernardi, Jörg R. Hörandel, A. G. Polatidis, Ashish Asgekar, A. Nelles, Angélica Sicard, H. Munk, R. J. van Weeren, Jason W. T. Hessels, D. McKay-Bukowski, I. de Pater, Matthias Hoeft, Oleg Smirnov, A. W. Gunst, Frank Breitling, Arthur Corstanje, Sebastien Hess, Quentin Nénon, Mark J. Bentum, J. van Leeuwen, R. C. Vermeulen, M. Loose, P. Zarka, H. J. A. Röttgering, P. Maat, M. J. Norden, M. Tagger, J. Moldón, F. de Gasperin, S. Bourdarie, Rene P. Breton, Annalisa Bonafede, John D. Swinbank, I. van Bemmel, Stephane Corbel, Martin Bell, V. I. Kondratiev, M. Pandey-Pommier, M. Iacobelli, James M. Anderson, Roberto Pizzo, Marcus Brüggen, Satyendra Thoudam, M. C. Toribio, Gerard H. Kuper, Antonia Rowlinson, Jochen Eislöffel, S. Duscha, Rebecca McFadden, M. A. Garrett, Daniel Santos-Costa, Julien N. Girard, Matthias Steinmetz, B. Ciardi, O. Wucknitz, J.-M. Grießmeier, M. Kuniyoshi, Ralph A. M. J. Wijers, Wilfred Frieswijk, Heino Falcke, C. Tasse, W. N. Brouw, S. Markov, Emanuela Orrú, H. Paas, Adam Deller, W. Reich, Dominik J. Schwarz, J. W. Broderick, E. Juette, G. Mann, Philip Best, C. Vocks, E. de Geus, Girard, J.N., Zarka, P., Tasse, C., Hess, S., De Pater, I., Santos-Costa, D., Nenon, Q., Sicard, A., Bourdarie, S., Anderson, J., Asgekar, A., Bell, M.E., Van Bemmel, I., Bentum, M.J., Bernardi, G., Best, P., Bonafede, A., Breitling, F., Breton, R.P., Broderick, J.W., Brouw, W.N., Brüggen, M., Ciardi, B., Corbel, S., Corstanje, A., De Gasperin, F., De Geus, E., Deller, A., Duscha, S., Eislöffel, J., Falcke, H., Frieswijk, W., Garrett, M.A., Grießmeier, J., Gunst, A.W., Hessels, J.W.T., Hoeft, M., Hörandel, J., Iacobelli, M., Juette, E., Kondratiev, V.I., Kuniyoshi, M., Kuper, G., Van Leeuwen, J., Loose, M., Maat, P., Mann, G., Markoff, S., McFadden, R., McKay-Bukowski, D., Moldon, J., Munk, H., Nelles, A., Norden, M.J., Orru, E., Paas, H., Pandey-Pommier, M., Pizzo, R., Polatidis, A.G., Reich, W., Röttgering, H., Rowlinson, A., Schwarz, D., Smirnov, O., Steinmetz, M., Swinbank, J., Tagger, M., Thoudam, S., Toribio, M.C., Vermeulen, R., Vocks, C., Van Weeren, R.J., Wijers, R.A.M.J., Wucknitz, O., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, ONERA - The French Aerospace Lab [Toulouse], ONERA, Netherlands Institute for Radio Astronomy (ASTRON), University of Southampton, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Jacobs University [Bremen], Leibniz-Institut für Astrophysik Potsdam (AIP), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Max Planck Institute for Astrophysics, Max-Planck-Gesellschaft, Radboud University [Nijmegen], Hamburger Sternwarte/Hamburg Observatory, Universität Hamburg (UHH), Thüringer Landessternwarte Tautenburg (TLS), Leiden Observatory [Leiden], Universiteit Leiden, Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Department of Pure Mathematics and Mathematical Statistics (DPMMS), Faculty of mathematics Centre for Mathematical Sciences [Cambridge] (CMS), University of Cambridge [UK] (CAM)-University of Cambridge [UK] (CAM), Ruhr-Universität Bochum [Bochum], Max-Planck-Institut für Radioastronomie (MPIFR), University of Oulu, University of Groningen [Groningen], Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CSIRO Astronomy and Space Science, Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Universität Bielefeld, Rhodes University, Grahamstown, Leibniz-Institut DSMZ-Deutsche Sammlung von Mikroorganismen und Zellkulturen GmbH / Leibniz Institute DSMZ-German Collection of Microorganisms and Cell Cultures (DSMZ), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011), European Project: 228261,EC:FP7:ERC,ERC-2008-AdG,SPARSEASTRO(2009), ITA, GBR, FRA, DEU, NLD, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Radboud university [Nijmegen], Universiteit Leiden [Leiden], Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Harvard University [Cambridge]-Smithsonian Institution, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), DPMMS/CMS, University of Cambridge [UK] (CAM), ANR-11-IDEX-0005-02/10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2011), Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Faculty of Science

Subjects
radio continuum: planetary systems, Brightness, 010504 meteorology & atmospheric sciences, radio continuum: planetary, EWI-27447, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, FOS: Physical sciences, Astrophysics, Electron, METIS-321662, 7. Clean energy, 01 natural sciences, Jupiter, symbols.namesake, 0103 physical sciences, Emission spectrum, IR-103183, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Radio continuum: planetary system, Planets and satellites: magnetic field, Astronomy and Astrophysics, LOFAR, Astronomy and Astrophysic, planets and satellites: magnetic fields, Spectral flux density, 13. Climate action, Space and Planetary Science, Van Allen radiation belt, Techniques: interferometric, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, systems, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Observing Jupiter's synchrotron emission from the Earth remains today the sole method to scrutinize the distribution and dynamical behavior of the ultra energetic electrons magnetically trapped around the planet (because in-situ particle data are limited in the inner magnetosphere). Aims. We perform the first resolved and low-frequency imaging of the synchrotron emission with LOFAR at 127 MHz. The radiation comes from low energy electrons (~1-30 MeV) which map a broad region of Jupiter's inner magnetosphere. Methods (see article for complete abstract) Results. The first resolved images of Jupiter's radiation belts at 127-172 MHz are obtained along with total integrated flux densities. They are compared with previous observations at higher frequencies and show a larger extent of the synchrotron emission source (>=4 $R_J$). The asymmetry and the dynamic of east-west emission peaks are measured and the presence of a hot spot at lambda_III=230 {\deg} $\pm$ 25 {\deg}. Spectral flux density measurements are on the low side of previous (unresolved) ones, suggesting a low-frequency turnover and/or time variations of the emission spectrum. Conclusions. LOFAR is a powerful and flexible planetary imager. The observations at 127 MHz depict an extended emission up to ~4-5 planetary radii. The similarities with high frequency results reinforce the conclusion that: i) the magnetic field morphology primarily shapes the brightness distribution of the emission and ii) the radiating electrons are likely radially and latitudinally distributed inside about 2 $R_J$. Nonetheless, the larger extent of the brightness combined with the overall lower flux density, yields new information on Jupiter's electron distribution, that may shed light on the origin and mode of transport of these particles., Comment: 10 pages, 12 figures, accepted for publication in A&A (27/11/2015) - abstract edited because of limited characters

Published
2015

31. Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra

Author

Norbert Krupp, Sarah V. Badman, Henrik Melin, Chihiro Tao, Laurent Lamy, Marina Galand, Sebastien Hess, and Graziella Branduardi-Raymont

Subjects
Physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics, medicine.disease_cause, Spectral line, Solar wind, Wavelength, Planet, Physics::Space Physics, medicine, Polar, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Ultraviolet
Abstract

The ionospheric response to auroral precipitation at the giant planets is reviewed, using models and observations. The emission processes for aurorae at radio, infrared, visible, ultraviolet, and X-ray wavelengths are described, and exemplified using ground- and space-based observations. Comparisons between the emissions at different wavelengths are made, where possible, and interpreted in terms of precipitating particle characteristics or atmospheric conditions. Finally, the spatial distributions and dynamics of the various components of the aurorae (moon footprints, low-latitude, main oval, polar) are related to magnetospheric processes and boundaries, using theory, in situ, and remote observations, with the aim of distinguishing between those related to internally-driven dynamics, and those related to the solar wind interaction.

Published
2015

32. Lead angles and emitting electron energies of Io-controlled decameter radio arcs

Author

Sebastien Hess, Baptiste Cecconi, Bertrand Bonfond, Philippe Zarka, A. Petin, University of Colorado, Laboratory for Atmospheric and Space Physics (LASP), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Laboratoire de Physique Atmosphérique et Planétaire, Université de Liège (LPAP)

Subjects
Physics, Flux tube, Field line, Plane (geometry), Astrophysics::High Energy Astrophysical Phenomena, Cyclotron, Astronomy, Astronomy and Astrophysics, Electron, Magnetic field, law.invention, Computational physics, Jupiter, Space and Planetary Science, law, Maser, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; The Io-controlled radio arcs are emissions in the decametric radio range which appear arc shaped in the time-frequency plane. Their occurrence is controlled by Io's position, so it has been for long inferred that they are powered by the Io-Jupiter electrodynamic interaction. Their frequency ranges correspond to the electron cyclotron frequencies along the Io Flux tube, so they are expected to be generated by cyclotron maser instability (CMI). The arc shape was proposed to be a consequence of the strong anisotropy of the decametric radio emissions beaming, combined with the topology of the magnetic field in the source and the observation geometry. Recent papers succeeded at reproducing the morphologies of a few typical radio arcs by modeling in three dimensions the observation geometry, using the best available magnetic field model and a beaming angle variation consistent with a loss-cone driven CMI. In the continuation of these studies, we present here the systematic modeling of a larger number of observations of the radio arcs emitted in Jupiter's southern hemisphere (including multiple arcs or arcs exhibiting abrupt changes of shape), which permits to obtain a statistical determination of the emitting field line localization (lead angle) relative to the instantaneous Io field line, and of the emitting particle velocities or energies. Variations of these parameters relative to Io's longitude are also measured and compared to the location of the UV footprints of the Io-Jupiter interaction. It is shown that the data are better organized in a reference frame attached to the UV spot resulting from the main Alfvén wing resulting from the Io-Jupiter interaction. It is proposed that the radio arcs are related to the first reflected Alfvén wing rather than to the main one.

Published
2010

33. Simulation of the Potential of a CubeSat designed for Accurate Plasma Measurement in LEO

Author

Oriol Jorba-Ferro, Thimothee Martens, Jean-Charles Mateo-Velez, Virginie Inguimber, Gael Murat, François Leblanc, Jean-Pierre Lebreton, Jean-Jacques Berthelier, Sebastien Hess, ONERA - The French Aerospace Lab [Toulouse], ONERA, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut Supérieur de l'Electronique et du Numérique - Lille (ISEN-Lille), Institut supérieur de l'électronique et du numérique (ISEN), Cardon, Catherine, and Institut supérieur de l'électronique et du numérique (ISEN)-Université catholique de Lille (UCL)

Subjects
Physics, Spacecraft, business.industry, Plasma parameters, Context (language use), Plasma, 7. Clean energy, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], symbols.namesake, [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Plasma Physics, Physics::Space Physics, symbols, Langmuir probe, Satellite, CubeSat, Aerospace engineering, business, ComputingMilieux_MISCELLANEOUS, Electron gun
Abstract

This paper presents the estimation of CubeSat charging in low Earth orbit (LEO) environment. The satellite will be equipped with a series of thin cylindrical Langmuir probes to access plasma parameters with a large temporal cadence. The electrostatic cleanliness basically requires the use of conductive surface elements to avoid differential charging and possible in homogeneities and disturbances of the plasma. However, this does not prevent the spacecraft to charge with respect to the neutral environment because electron mobility is much larger than ions', and also due to the wake effect created by supersonic ions combined with the satellite geometry. In this context, the thin sheath theory is only approximate at getting the plasma parameters. This paper presents efforts to estimate numerically charging levels of a typical CubeSat using the Spacecraft Plasma Interaction Software (SPIS). It also presents preliminary experiments of a mock-up equipped with Langmuir probes and with an electron emitter.

Published
2015

34. Simulations of plasma thruster effect on the electrostatic behavior of spacecrafts in GEO

Author

Jean-Charles Mateo-Velez, Sebastien Hess, and Pierre Sarrailh

Subjects
Physics, Work (thermodynamics), Electrostatic discharge, Spacecraft, business.industry, Plasma, Plume, Physics::Plasma Physics, Phase (matter), Physics::Space Physics, Orbit (dynamics), Aerospace engineering, Material properties, business
Abstract

This paper presents a study of the possible effects of the all-electric technology for orbit transfer on the electrostatic behavior. This work focuses on the effect of the plume interaction with the spacecraft and its effect on the electrostatic behavior in GEO. After a first phase of assessment of the plasma interactions spacecraft, the effect of the plasma collection has been estimated in term of contamination, erosion and material properties change. Finally, the consequences of these material property changes in term of charging and electrostatic discharge have been shown. This permits a preliminary analysis of the influence of the all electric transfer phase on the GEO operations.

Published
2015

35. Variability of the hydrogen in the martian upper atmosphere as simulated by a 3D atmosphere–exosphere coupling

Author

Francisco Gonzalez-Galindo, François Leblanc, Miguel Lopez-Valverde, François Forget, Ronan Modolo, Jean-Yves Chaufray, Sebastien Hess, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], 010504 meteorology & atmospheric sciences, Hydrogen, Atmosphere, Northern Hemisphere, chemistry.chemical_element, Mars, Astronomy and Astrophysics, Atmospheric sciences, 01 natural sciences, Corona, Solar cycle, chemistry, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Environmental science, Solstice, Thermosphere, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Exosphere
Abstract

International audience; We present the temporal variability of the atomic and molecular hydrogen density derived from a 3D General Circulation Model describing the Martian atmosphere from the surface to the exobase. A kinetic exospheric model is used to compute the hydrogen density above the exobase. We use these models to study the diurnal and seasonal variations of the hydrogen density and the Jeans escape rate as well as their variations with solar activity, assuming a classic dust scenario. We find that the diurnal variations of the hydrogen density are important with a peak in the dawn region during equinoxes and a peak on the nightside during solstices. These features result from the dynamics of the Martian upper atmosphere. The variations of the atomic hydrogen Jeans escape with seasons and solar activity are in the range 1.3x1025 s-1 – 4.4x1026 s-1. A factor ∼8 is due to the seasonal variations with a maximum during the winter solstice in the northern hemisphere and a minimum during the summer solstice in the northern hemisphere that we attribute to the variation of the Mars-Sun distance. A factor ∼5 is due to the solar cycle with a maximum escape rate at high solar activity. The variations of the molecular hydrogen Jeans escape with seasons and solar activity are in the range 3x1022 s-1 – 6x1024 s-1. A factor ∼10 is due to the seasonal variations with a maximum during the winter solstice in the northern hemisphere and a minimum during the summer solstice in the northern hemisphere. A factor ∼20 is due to the solar cycle with a maximum escape rate at high solar activity. If Jeans escape is the major escape channel for hydrogen, the hydrogen escape is never limited by diffusion. The hydrogen density above 10,000 km presents seasonal and solar cycle variations similar to the Jeans escape rate at all latitudes and local times. This 3D temporal model of the hydrogen thermosphere/exosphere will be useful to interpret future MAVEN observations and the consequences of the hydrogen corona variability on the Martian plasma environment.

Published
2015

36. The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets

Author

Roberto Peron, Jonathan J. Fortney, Denis Grodent, Ralf Srama, L. Lamy, Robert Ebert, S. Hsu, Ioannis A. Daglis, Edward C. Sittler, K. Konstantinidis, Matthew S. Tiscareno, O. Karatekin, M. H. Hofstadter, Nicolas Rambaux, Matthew M. Hedman, Richard Holme, Andrew J. Coates, Tom Stallard, Pierre Henri, Sarah V. Badman, Bruno Christophe, Jessica Agarwal, M. I. Desai, Diego Turrini, Fritz M. Neubauer, Andrew Smith, Agustín Sánchez-Lavega, Julianne I. Moses, Davide Grassi, G. S. Orton, O. Mousis, N. André, C. Labrianidis, Mihaly Horanyi, Federico Tosi, Henrik Melin, P. Zarka, Mathew J. Owens, S. M. P. McKenna-Lawlor, Elizabeth P. Turtle, Benoît Noyelles, Shawn M. Brooks, Matthieu Laneuville, Richard M. Ambrosi, John F. Cooper, Dominic Dirkx, Caitriona M. Jackman, Mario M. Bisi, C. Bracken, Kevin H. Baines, Harald Krüger, Mathieu Barthelemy, E. Khalisi, Kunio M. Sayanagi, Pontus Brandt, Tom Nordheim, J. L. MacArthur, Ondrej Santolik, Glyn Collinson, Sascha Kempf, Jürgen Blum, Robert W. Wilson, I. de Pater, Veerle Sterken, William S. Kurth, Patrick G. J. Irwin, Craig B. Agnor, Frank Postberg, T. M. Bocanegra-Bahamón, Jon K. Hillier, Julie Castillo-Rogez, Eberhard Grün, Georg Moragas-Klostermeyer, Michele K. Dougherty, Christelle Briois, Christopher T. Russell, Nicholas Achilleos, Bertrand Bonfond, Mario Trieloff, Kurt D. Retherford, Abigail Rymer, Renaud Sallantin, Christina Plainaki, Frank Spahn, N. Nettelmann, Achim Morschhauser, S. Vinatier, Gabriel Tobie, Serge Reynaud, Elias Roussos, I. Gerth, A. Luntzer, Joachim Saur, M. Costa-Sitja, Paul M. Schenk, Ravit Helled, David M. Lucchesi, C. Briand, J. Schubert, Régis Courtin, George Hospodarsky, Thibault Cavalié, Sebastien Hess, Chris S. Arridge, V. Lainey, Adam Masters, Anna Milillo, Gianrico Filacchione, Andrea Maier, Jacques Gustin, Nick Sergis, Zoltan Sternovsky, Don Banfield, Leigh N. Fletcher, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Department of Physics and Astronomy [UCL London], European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Queen Mary University of London (QMUL), Space Research Centre [Leicester], University of Leicester, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institute of Space and Astronautical Science (ISAS), Department of Physics [Lancaster], Lancaster University, Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, University of Wisconsin-Madison, Cornell University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Technische Universität Braunschweig [Braunschweig], Delft University of Technology (TU Delft), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, National University of Ireland Maynooth (NUIM), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de physique et chimie de l'environnement (LPCE), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, DPHY, ONERA, Université Paris Saclay [Châtillon], ONERA-Université Paris-Saclay, NASA Goddard Space Flight Center (GSFC), European Space Astronomy Centre (ESAC), Department of Physics [Athens], National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Southwest Research Institute [San Antonio] (SwRI), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], University of California [Santa Cruz] (UCSC), University of California, Max-Planck-Institut für Kernphysik (MPIK), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], University of Idaho [Moscow, USA], Tel Aviv University [Tel Aviv], HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg], School of Environmental Sciences [Liverpool], University of Liverpool, University of Iowa [Iowa City], Department of Physics [Oxford], School of Physics and Astronomy [Southampton], University of Southampton, Royal Observatory of Belgium [Brussels], University of Stuttgart, Universität der Bundeswehr München [Neubiberg], Department of Physics and Astronomy [Iowa City], UTesat-Spacecom, Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), University of Vienna [Vienna], Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Space Technology Ireland Limited, Institut für Raumfahrtsysteme (IRS), Universität Stuttgart [Stuttgart], Deutsches Zentrum für Luft- und Raumfahrt (DLR), Space Science Institute [Boulder] (SSI), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Institute for Geophysics and Meteorology [Köln] (IGM), University of Cologne, Université de Namur [Namur], University of Reading (UOR), Université Pierre et Marie Curie - Paris 6 - UFR de Médecine Pierre et Marie Curie (UPMC), Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire Kastler Brossel (LKB (Jussieu)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, University of the Basque Country [Bizkaia] (UPV/EHU), Institute of Atmospheric Physics, Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (ASCR), Lunar and Planetary Institute [Houston] (LPI), Department of Earth Sciences [USC Los Angeles], University of Southern California (USC), Office for Space Research and Applications [Athens], Academy of Athens, University of Potsdam, Max Planck Institute for Nuclear Physics (MPIK), International Space Science Institute [Bern] (ISSI), Cornelle University, Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Agence Spatiale Européenne = European Space Agency (ESA), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), NASA-California Institute of Technology (CALTECH), Cornell University [New York], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], National University of Ireland Maynooth (Maynooth University), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), DPHY, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), National and Kapodistrian University of Athens (NKUA), University of Oxford, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Tel Aviv University (TAU), HELIOS - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University, Royal Observatory of Belgium [Brussels] (ROB), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Université de Namur [Namur] (UNamur), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Universität zu Köln = University of Cologne, Czech Academy of Sciences [Prague] (CAS), University of Potsdam = Universität Potsdam, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Centre for Planetary Sciences [UCL/Birkbeck] ( CPS ), European Space Research and Technology Centre ( ESTEC ), European Space Agency ( ESA ), Queen Mary University of London ( QMUL ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Space and Astronautical Science ( ISAS ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), University of Wisconsin-Madison [Madison], Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Delft University of Technology ( TU Delft ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), National University of Ireland Maynooth ( NUIM ), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] ( APL ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique et chimie de l'environnement ( LPCE ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), ONERA - The French Aerospace Lab ( Toulouse ), ONERA, NASA Goddard Space Flight Center ( GSFC ), European Space Astronomy Center ( ESAC ), National and Kapodistrian University of Athens, University of California [Berkeley], Southwest Research Institute [San Antonio] ( SwRI ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Istituto Nazionale di Astrofisica ( INAF ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of California [Santa Cruz] ( UCSC ), Max-Planck-Institut für Kernphysik ( MPIK ), Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), University of Iowa [Iowa], University of Southampton [Southampton], Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Institut für Raumfahrtsysteme ( IRS ), Deutsches Zentrum für Luft- und Raumfahrt ( DLR ), Space Science Institute [Boulder] ( SSI ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Institute for Geophysics and Meteorology [Köln] ( IGM ), University of Reading ( UOR ), Université Pierre et Marie Curie - Paris 6 - UFR de Médecine Pierre et Marie Curie ( UPMC ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Laboratoire Kastler Brossel ( LKB (Jussieu) ), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris ( FRDPENS ), Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ) -École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Institute of Geophysics and Planetary Physics [Los Angeles] ( IGPP ), University of California at Los Angeles [Los Angeles] ( UCLA ), University of the Basque Country [Bizkaia] ( UPV/EHU ), Institute of Atmospheric Physics [Prague] ( IAP ), Czech Academy of Sciences [Prague] ( ASCR ), Lunar and Planetary Institute [Houston] ( LPI ), Department of Earth Sciences [Los Angeles], University of Southern California ( USC ), Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), and International Space Science Institute ( ISSI )

Subjects
Outer planets, Gas giant, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Uranus, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Natural satellites, Astrobiology, ice giant planets, Neptune, Rings, Physics, Naturalsatellites, Atmosphere, Nice model, Institut für Physik und Astronomie, Astronomy, Astronomy and Astrophysics, orbital mission, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], science case, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Rings of Uranus, Space and Planetary Science, Exploration of Uranus, Magnetosphere, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Planetary interior, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Ice giant
Abstract

著者人数: 114名, Accepted: 2014-08-07, 資料番号: SA1005021000

Published
2014

37. Three-dimensional Martian ionosphere model: II. Effect of transport processes due to pressure gradients

Author

François Forget, Jean-Yves Chaufray, Miguel Lopez-Valverde, Ronan Modolo, Olivier Witasse, Pierre-Louis Blelly, F. Gonzalez-Galindo, Sebastien Hess, Manabu Yagi, François Leblanc, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut Pierre-Simon-Laplace (IPSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC), Planetary Plasma and Atmospheric Research Center [Sendai] (PPARC), Tohoku University [Sendai], Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and European Space Agency (ESA)

Subjects
Martian, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Mars, Mars Exploration Program, Atmospheric sciences, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Solar cycle, Physics::Geophysics, Dynamics, Atmosphere, Solar wind, Geophysics, Flow velocity, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Physics::Space Physics, Earth and Planetary Sciences (miscellaneous), Environmental science, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Pressure gradient, Physics::Atmospheric and Oceanic Physics
Abstract

International audience; To study the transport of the ionospheric plasma on Mars, we have included a 3D multifluid dynamical core in a Martian General Circulation Model (GCM). Vertical transport modifies the ion density above ~160 km on the dayside, especially the ions produced at high altitudes like O+, N+ and C+. Near the exobase, the dayside to nightside flow velocity reaches few hundreds of m/s, due to a large horizontal pressure gradient. Comparison with MEX/ASPERA-3 measurements between 290 - 500 km, suggests this flow could account for at least 20% of the flow produced by the solar wind. This flow is not sufficient to populate substantially the nightside ionosphere at high altitudes, in agreement with recent observations, because of a strong nightside downward flow produced by vertical pressure gradient. The O2+ and NO+ ion densities on the nightside at low altitudes (~130 km) are modified by this downward flow, compared to simulated densities without ion dynamics, while other ions are lost by chemical reactions. Variability at different time scales (diurnal, seasonal and solar cycle) are studied. We simulate diurnal and seasonal variations of the ionospheric composition due to the variability of the neutral atmosphere and solar flux at the top of the atmosphere. The ionospheric dynamics are not strongly affected by seasons and solar cycles and the retroaction of the ionosphere on the neutral atmosphere temperature and velocity is negligible compared to other physical processes below the exobase.

Published
2014

38. Evolution of the Io footprint brightness I: Far-UV observations

Author

Aikaterini Radioti, Virginie Chantry, Joachim Saur, Sebastien Hess, Sven Jacobsen, Jean-Claude Gérard, Denis Grodent, John Clarke, Bertrand Bonfond, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Institut für Geophysik und Meteorologie [Köln], Universität zu Köln, Research and Technology Centre Westcoast, Christian-Albrechts-Universität zu Kiel (CAU), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), and Universität zu Köln = University of Cologne

Subjects
Brightness, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnetosphere, Io, 01 natural sciences, Jovian, 010305 fluids & plasmas, Jupiter, Atmosphere, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Hubble space telescope, 0105 earth and related environmental sciences, Physics, Aurora, Astronomy, Astronomy and Astrophysics, Torus, Plasma, Io footprint, 13. Climate action, Space and Planetary Science, Longitude
Abstract

International audience; The Io footprint (IFP) is a set of auroral spots and an extended tail resulting from the strong interaction between Io and the Jovian magnetosphere. For the first time, we present measurements of the brightness and precipitated power for each individual spot, using the image database gathered from 1997 to 2009 with the Hubble Space Telescope in the Far-UV domain. We show that the relative brightness of the spots varies with the System III longitude of Io. Moreover, our novel measurement method based on 3D simulations of the auroral features allows to derive the precipitated energy fluxes from images on which the emission region is observed at a slant angle. Peak values as high as 2 W/m2 are observed for the main spot, probably triggering a localized and sudden heating of the atmosphere. Additionally, strong brightness differences are observed from one hemisphere to another. This result indicates that the location of Io in the plasma torus is not the only parameter to control the brightness, but that the magnetic field asymmetries also play a key role. Finally, we present new data confirming that significant variations of the spots' brightness on timescales of 2-4 minutes are ubiquitous, which suggests a relationship with intermittent double layers close to Jovian surface.

Published
2013

39. How could the Io footprint disappear?

Author

Peter Delamere, Bertrand Bonfond, Sebastien Hess, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], and University of Alaska [Fairbanks] (UAF)

Subjects
Brightness, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Magnetosphere, Astrophysics, 01 natural sciences, Jovian, Jupiter, UV aurora, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Dispersive Alfvén waves, Astronomy and Astrophysics, Torus, Plasma, Geophysics, Io footprint, Amplitude, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Jupiter-Io interaction, Ionosphere
Abstract

International audience; The interaction of Io with the Jovian magnetosphere is the best known - and the most intense - case of satellite-magnetosphere interaction. The interaction involves a power of more than a TeraWatt, a few percent of which are transferred to electrons. These electrons precipitate in the Jovian ionosphere where they light-up bright auroral emissions (several 100's kR to a few 1000's kR). The brightness of the Io-controlled UV auroras is known to vary, due to the Jovian magnetic field tilt, which induces longitudinal variations, and due to the Io torus ever changing parameters (possibly due to Io's volcanic activity), which induce a temporal variation. As Io-controlled UV auroras have been monitored for a long time, the variation of their brightness is well-documented, and the typical amplitude of these variations has been established. However, on June, 7th 2012 an unusual event occurred in the plasma torus surrounding Io, which triggered its own UV emissions on Jupiter in a region mapping to Io's orbit. When Io reached that region, Io's auroral footprint disappeared, its brightness dimming by at least a factor of three to be below the background aurora brightness. Both the auroral event at such a low latitude and the Io footprint disappearance are events that have never been observed before and should be quite rare. However, the question of how the bright Io footprint becomes that weak remains. From a theoretical point-of-view, the Io-Jupiter interaction has been widely studied. In the 80's, it was shown that Alfvén waves are radiated from Io, carrying currents to Jupiter. In the late-2000's, studies showed that dispersive Alfvén waves were likely to cause the acceleration of the electrons powering the auroral emissions, although Io-scale Alfvén waves should be non-dispersive. More recently, a model was built which permits one to compute the ratio between dispersive and non-dispersive waves in the auroral region for satellite-magnetosphere interactions, and thus the brightness of the related aurorae. We use this model to investigate which variation of the interaction parameters could lead to the Io footprint disappearance.

Published
2013

40. The multiple spots of the Ganymede auroral footprint

Author

Denis Grodent, Fran Bagenal, Bertrand Bonfond, Jacques Gustin, Jean-Claude Gérard, Aikaterini Radioti, Sebastien Hess, John Clarke, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Center for Space Physics [Boston] (CSP), and Boston University [Boston] (BU)

Subjects
010504 meteorology & atmospheric sciences, Magnetosphere, 01 natural sciences, Astrobiology, Jupiter, Footprint, Planet, Ganymede, 0103 physical sciences, Enceladus, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, geography, geography.geographical_feature_category, Plasma sheet, Astronomy, footprint, aurora, Geophysics, Volcano, 13. Climate action, General Earth and Planetary Sciences, Ionosphere, Geology
Abstract

International audience; The interaction between the moons and the magnetosphere of giant planets sometimes gives rise to auroral signatures in the planetary ionosphere, called the satellite footprints. So far, footprints have been detected for Io, Europa, Ganymede and Enceladus. These footprints are usually seen as single spots. However, the Io footprint, the brightest one, displays a much more complex morphology made of at least three different spots and an extended tail. Here, we present Hubble Space Telescope FUV images showing evidence for a second spot in the Ganymede footprint. The spots separation distance changes as Ganymede moves latitudinally in the plasma sheet, as is seen for the Io footprint. This indicates that the processes identified at Io are universal. Moreover, for similar Ganymede System III longitudes, the distance may also vary significantly with time, indicating changes in the plasma sheet density. We identified a rapid evolution of this distance ~8 days after the detection of a volcanic outburst at Io, suggesting that such auroral observations could be used to estimate the plasma density variations at Ganymede.

Published
2013

41. Evolution of the Io footprint brightness II: Modeling

Author

Aikaterini Radioti, Bertrand Bonfond, Jean-Claude Gérard, Denis Grodent, Sven Jacobsen, Sebastien Hess, Virginie Chantry, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Department of Space Studies [Boulder], Southwest Research Institute [Boulder] (SwRI), Institut d'Astrophysique et de Géophysique [Liège], Institut für Geophysik und Meteorologie [Köln], Universität zu Köln = University of Cologne, Research and Technology Centre Westcoast, Christian-Albrechts-Universität zu Kiel (CAU), and Universität zu Köln

Subjects
Solar System, Brightness, Io-Jupiter interaction, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Electron precipitation, Magnetosphere, Astrophysics, 01 natural sciences, 7. Clean energy, Jovian, Jupiter, Alfvén wave, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Astronomy, Astronomy and Astrophysics, Electron acceleration, Alfvén waves, Io footprint, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Ionosphere
Abstract

International audience; The interaction of Io with the Jovian magnetosphere creates the best known and brightest satellite-controlled aurorae in our solar system. These aurorae are generated by the precipitation of electrons, which are accelerated by the Alfvén waves carrying the current between the satellite and the planet. A recent study computed the energy deposited on top of Jupiter's ionosphere due to the electron precipitation and retrieved the correct mean brightness of Io-related aurorae. The model developed in this study takes into account the acceleration mechanism and the Alfvén wave propagation effects. We use the same method to investigate the brightness variation of the different components of the Io footprint as a function of longitude. These observations are discussed in a companion paper. We identify several effects that act together to modulate the footprint brightness such as Alfvén wave reflections, magnetic mirroring of the electrons, the local interaction at Io and kinetic effects close to Jupiter. We identify the effects contributing the most to the modulation of the brightnesses of the three brightest components of the Io footprints: the main and reflected Alfvén wing spots and the transhemispheric electron spot. We show in particular that the modulation of the efficiency of the electron acceleration can be of greater importance than the modulation of the power generated at Io. We reproduce the average modulation of the spot brightnesses and present an extensive discussion of possible explanations for the observed features not reproduced by our model.

Published
2013

42. A global hybrid model for Mercury's interaction with the solar wind: Case study of the dipole representation

Author

Gérard Chanteur, François Leblanc, Ronan Modolo, Emilie Richer, and Sebastien Hess

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Field line, Soil Science, Magnetosphere, Aquatic Science, Oceanography, 01 natural sciences, Magnetosheath, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Mercury's magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Paleontology, Forestry, Geophysics, Dipole model of the Earth's magnetic field, Computational physics, Magnetic field, Solar wind, Dipole, Space and Planetary Science, Physics::Space Physics
Abstract

The interaction of the solar wind (SW) with the magnetic field of Mercury is investigated by means of a three dimensional parallelized multispecies hybrid model. A comparison between two mathematical representations of Mercury's intrinsic magnetic field is studied. The first model is an Offset Dipole (OD) having the offset and dipolar moment reported by Anderson et al. (2011). The second model is a combination of a Dipole and a Quadrupole (DQ), the total field is fitted to the offset dipolar field, for northern latitudes greater than 50°. Simulations reproduce the features which characterize Mercury's interaction with the SW, encompassing the Bow Shock (BS), the magnetosheath, the magnetotail, the "cusps" region and the neutral current sheet. Global hybrid simulations of the Hermean magnetosphere run for the OD and DQ models demonstrate that the southern parts of the magnetospheres produced by the OD and DQ models differ greatly in topology and volume meanwhile their northern parts-are quite similar. In particular the DQ model exhibits a dome of closed field lines around the south pole in contrast to the OD. Without further information on the intrinsic magnetic field of the planet in the southern region which should be provided by BepiColombo after year 2020, we can only speculate on the influence of the different magnetic topologies on the magnetospheric dynamics.

Published
2012

43. Comment on 'Jovian slow-drift shadow events' by T. Koshida et al

Author

Ph. Zarka, Sebastien Hess, and Fabrice Mottez

Subjects
Physics, Atmospheric Science, 010504 meteorology & atmospheric sciences, Ecology, Paleontology, Soil Science, Astronomy, Forestry, Aquatic Science, Oceanography, 01 natural sciences, Jovian, Jupiter, Geophysics, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Shadow, Earth and Planetary Sciences (miscellaneous), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth-Surface Processes, Water Science and Technology, Plasma density
Abstract

] Koshidaetal.[2010a]describespecificunusualfeaturesof the Jovian decametric (DAM) radiation, called “slow-driftshadow” (SDS) events. These events consist of brief (a fewtens of milliseconds long) extinctions of the slowly varyingIo-induced Jovian decametric emission (so-called«L-burst»)in the 21–23 MHz range. SDS drifts from high to low fre-quencies across the observed 21–23 MHz range in a fewhundred milliseconds.

Published
2012

44. Natural radio emission of Jupiter as interferences for radar investigations of the icy satellites of Jupiter

Author

Baptiste Cecconi, Donald D. Blankenship, Lorenzo Bruzzone, Alain Herique, Daniel Santos-Costa, Wlodek Kofman, Jean-Louis Bougeret, Giovanni Alberti, Sebastien Hess, M. R. Santovito, Ph. Zarka, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Helmholtz zentrum für Schwerionenforschung GmbH (GSI), UJF-Grenoble I/CNRS, Université Joseph Fourier - Grenoble 1 (UJF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Faculty of Environment and Natural Resources, University of Freiburg [Freiburg], University of Trento [Trento], Ingénieurs, Techniciens et Administratifs, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Physique des plasmas

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Radio spectrum, Jovian, law.invention, Radio telescope, Jupiter, symbols.namesake, Exploration of Jupiter, law, 0103 physical sciences, Radar, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Remote sensing, Physics, [PHYS]Physics [physics], Europa Orbiter, Astronomy, Astronomy and Astrophysics, Galilean moons, 13. Climate action, Space and Planetary Science, Physics::Space Physics, symbols, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Radar instruments are part of the core payload of the two Europa Jupiter System Mission (EJSM) spacecraft: NASA-led Jupiter Europa Orbiter (JEO) and ESA-led Jupiter Ganymede Orbiter (JGO). At this point of the project, several frequency bands are under study for radar, which ranges between 5 and 50 MHz. Part of this frequency range overlaps with that of the natural jovian radio emissions, which are very intense in the decametric range, below 40 MHz. Radio observations above 40 MHz are free of interferences, whereas below this threshold, careful observation strategies have to be investigated. We present a review of spectral intensity, variability and sources of these radio emissions. As the radio emissions are strongly beamed, it is possible to model the visibility of the radio emissions, as seen from the vicinity of Europa or Ganymede. We have investigated Io-related radio emissions as well as radio emissions related to the auroral oval. We also review the radiation belts synchrotron emission characteristics. We present radio sources visibility products (dynamic spectra and radio source location maps, on still frames or movies), which can be used for operation planning. This study clearly shows that a deep understanding of the natural radio emissions at Jupiter is necessary to prepare the future EJSM radar instrumentation. We show that this radio noise has to be taken into account very early in the observation planning and strategies for both JGO and JEO. We also point out possible synergies with RPW (Radio and Plasma Waves) instrumentations.

Published
2012

45. Planetary and exoplanetary low frequency radio observations from the Moon

Author

Philippe Zarka, Laurent Lamy, Baptiste Cecconi, J.-L. Bougeret, Sebastien Hess, C. Briand, David Mimoun, Amin Aminaei, Heino Falcke, A. A. Konovalenko, Julien N. Girard, J.-M. Grießmeier, Marc Klein-Wolt, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Radio Astronomy of NASU [Kharkiv] (IRA), National Academy of Sciences of Ukraine (NASU), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), and Radboud university [Nijmegen]-Radboud university [Nijmegen]

Subjects
Thermal noise, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astronomy, Hot Jupiters, Uranus, Exoplanetology, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Planets, 01 natural sciences, Lightning, Astrobiology, Jupiter, Neptune, Planet, Saturn, 0103 physical sciences, Hot Jupiter, Radio emission, Moon, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Aurora, Lunar radio array, Galactic background, Exoplanets, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Goniopolarimetry, Exoplanet, 13. Climate action, Space and Planetary Science, Magnetosphere, Physics::Space Physics, Radioastronomy, Astrophysics::Earth and Planetary Astrophysics
Abstract

International audience; We analyze the planetary and exoplanetary science that can be carried out with precursor as well as future low frequency radio instruments on the Moon, assessing the limiting noise sources, comparing them to the average and peak spectra of all planetary radio components as they will be seen from the Lunar surface or orbit. We identify which objectives will be accessible with each class of instrument, and discuss the interest of these observations compared to observations by planetary probes and to ground-based observations by large low-frequency radio arrays. The interest of goniopolarimetry is emphasized for pathfinder missions.

Published
2012

46. Uranus Pathfinder: exploring the origins and evolution of Ice Giant planets

Author

Abigail Rymer, S. Kemble, Elias Roussos, Sebastien Hess, Benoît Noyelles, Imke de Pater, Nick Sergis, Glyn Collinson, Stas Barabash, Ravit Helled, Jared Leisner, Chris S. Arridge, Nicholas A Teanby, Baptiste Cecconi, Andy F. Cheng, Norbert Krupp, Andrew Bacon, Joachim Saur, Yves Langevin, Andrew Fazakerley, Steve Miller, Jaques Gustin, Matthew S. Tiscareno, Christopher T. Russell, Mathieu Barthelemy, Nadine Nettelmann, Richard Holme, Philippe Zarka, Ingo Müller-Wodarg, Apostolos A. Christou, Andrew J. Coates, Robert Ebert, Thomas P. Andert, Olivier Mousis, Sandrine Vinatier, Paul M. Schenk, Gerald Schubert, Laurent Lamy, Michael Guest, Craig B. Agnor, Régis Courtin, Daniel Gautier, Jan-Erik Wahlund, Cesar Bertucci, Ulrich R. Christensen, Pontus Brandt, Javier Martin-Torres, Adam Masters, Don Banfield, Silvia Tellmann, Elizabeth P. Turtle, Matthew M. Hedman, Frank Sohl, Mark Hofstadter, Leigh N. Fletcher, Özgür Karatekin, Chris Paranicas, Kunio M. Sayanagi, Nicolas André, Agustín Sánchez-Lavega, Tom Stallard, Kevin H. Baines, Eric Quémerais, Martin Pätzold, Supriya Chakrabarti, Marina Galand, L. Peacocke, Pierre Henri, John F. Cooper, Gabriel Tobie, Marta Entradas, Nicholas Achilleos, Michele K. Dougherty, Renée Prangé, C. P. Chaloner, Henrik Melin, Geraint H. Jones, Jonathan J. Fortney, Edward C. Sittler, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), School of Physics and Astronomy [London], Queen Mary University of London (QMUL), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), University of Rostock [Germany], Institute of Geophysics and Planetary Physics [Los Angeles] (IGPP), University of California [Los Angeles] (UCLA), University of California-University of California, Department of Physics and Astronomy [Leicester], University of Leicester, Cornell University, Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Astrium [Stevenage], EADS - European Aeronautic Defense and Space, Department of Physics and Astronomy [UCL London], Universität der Bundeswehr München [Neubiberg], Swedish Institute of Space Physics [Uppsala] (IRF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Universidad de Buenos Aires [Buenos Aires] (UBA)-Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Armagh Observatory [Armagh], NASA Goddard Space Flight Center (GSFC), Blackett Laboratory, Imperial College London, Southwest Research Institute [San Antonio] (SwRI), Department of Science and Technology Studies [London] (STS), University of California [Santa Cruz] (UCSC), University of California, Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Department of Earth and Space Sciences [Los Angeles], University of Colorado [Boulder], School of Environmental Sciences [Liverpool], University of Liverpool, Royal Observatory of Belgium [Brussels], University of Iowa [Iowa City], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Space Research Centre [Leicester], Fondation Universitaire Notre Dame de la Paix (FUNDP), Facultés Universitaires Notre-Dame de la Paix, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy [Berkeley], University of California [Berkeley], Rhenish Institute for Environmental Research (RIU), University of Cologne, HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Institute for Geophysics and Meteorology [Köln] (IGM), Lunar and Planetary Institute [Houston] (LPI), Office for Space Research and Applications [Athens], Academy of Athens, DLR Institute of Planetary Research, German Aerospace Center (DLR), School of Earth Sciences [Bristol], University of Bristol [Bristol], Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Oxford, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of Rostock, University of California (UC)-University of California (UC), Cornell University [New York], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Royal Observatory of Belgium [Brussels] (ROB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Facultés Universitaires Notre Dame de la Paix (FUNDP), University of California [Berkeley] (UC Berkeley), HELIOS - LATMOS, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, California Institute of Technology (CALTECH)-NASA, Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Universität der Bundeswehr München [Neubiberg] = Bundeswehr University, Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Queen Mary University of London ( QMUL ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Institute of Geophysics and Planetary Physics [Los Angeles] ( IGPP ), University of California at Los Angeles [Los Angeles] ( UCLA ), Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Institut de Planétologie et d'Astrophysique de Grenoble ( IPAG ), Observatoire des Sciences de l'Univers de Grenoble ( OSUG ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astronomia y Fisica del Espacio ( IAFE ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ) -Universidad de Buenos Aires [Buenos Aires], Johns Hopkins University Applied Physics Laboratory [Laurel, MD] ( APL ), Center for Space Physics [Boston] ( CSP ), Boston University [Boston] ( BU ), Max Planck Institute for Solar System Research ( MPS ), NASA Goddard Space Flight Center ( GSFC ), Southwest Research Institute [San Antonio] ( SwRI ), Department of Science and Technology Studies [London] ( STS ), University of California [Santa Cruz] ( UCSC ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), University of Colorado Boulder [Boulder], University of Iowa [Iowa], Centro de Astrobiologia [Madrid] ( CAB ), Instituto Nacional de Técnica Aeroespacial ( INTA ) -Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Fondation Universitaire Notre Dame de la Paix ( FUNDP ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Astronomy Department [Berkeley], Rhenish Institute for Environmental Research ( RIU ), Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), University of the Basque Country/Euskal Herriko Unibertsitatea ( UPV/EHU ), Institute for Geophysics and Meteorology [Köln] ( IGM ), Lunar and Planetary Institute [Houston] ( LPI ), and German Aerospace Center ( DLR )

Subjects
Solar System, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Ciencias Físicas, Uranus, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], interior, Natural satellite, 7. Clean energy, 01 natural sciences, Astrobiology, Ice Giant, Orbiter, Neptune, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, ICE GIANT, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], natural satellite, ice giants, Nice model, Giant planet atmosphere, Astronomy, Astronomy and Astrophysics, Planetary system, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Ring system, Dynamo, Astronomía, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], URANUS, 13. Climate action, Space and Planetary Science, Exploration of Uranus, Magnetosphere, GIANT PLANET ATMOSPHERE, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ORBITER, CIENCIAS NATURALES Y EXACTAS, Ice giant
Abstract

The “Ice Giants” Uranus and Neptune are a different class of planet compared to Jupiter and Saturn. Studying these objects is important for furthering our understanding of the formation and evolution of the planets, and unravelling the fundamental physical and chemical processes in the Solar System. The importance of filling these gaps in our knowledge of the Solar System is particularly acute when trying to apply our understanding to the numerous planetary systems that have been discovered around other stars. The Uranus Pathfinder (UP) mission thus represents the quintessential aspects of the objectives of the European planetary community as expressed in ESA’s Cosmic Vision 2015–2025. UP was proposed to the European Space Agency’s M3 call for medium-class missions in 2010 and proposed to be the first orbiter of an Ice Giant planet. As the most accessible Ice Giant within the M-class mission envelope Uranus was identified as the mission target. Although not selected for this call the UP mission concept provides a baseline framework for the exploration of Uranus with existing low-cost platforms and underlines the need to develop power sources suitable for the outer Solar System. The UP science case is based around exploring the origins, evolution, and processes at work in Ice Giant planetary systems. Three broad themes were identified: (1) Uranus as an Ice Giant, (2) An Ice Giant planetary system, and (3) An asymmetric magnetosphere. Due to the long interplanetary transfer from Earth to Uranus a significant cruise-phase science theme was also developed. The UP mission concept calls for the use of a Mars Express/Rosetta-type platform to launch on a Soyuz–Fregat in 2021 and entering into an eccentric polar orbit around Uranus in the 2036–2037 timeframe. The science payload has a strong heritage in Europe and beyond and requires no significant technology developments. Fil: Arridge, Christopher S.. University College London; Estados Unidos Fil: Agnor, Craig B.. Queen Mary University of London; Reino Unido Fil: Andre, Nicolas. Centre National de la Recherche Scientifique; Francia Fil: Baines, Kevin H.. National Aeronautics And Space Administration; Estados Unidos Fil: Fletcher, Leigh N.. University of Oxford; Reino Unido Fil: Gautier, Daniel. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Hofstadter, Mark D.. National Aeronautics And Space Administration; Estados Unidos Fil: Jones, Geraint H.. University College London; Estados Unidos Fil: Lamy, Laurent. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Langevin, Yves. Centre National de la Recherche Scientifique; Francia Fil: Mousis, Olivier. Centre National de la Recherche Scientifique; Francia Fil: Nettelmann, Nadine. Universitat Rostock; Alemania Fil: Russell, Christopher T.. University of California at Los Angeles; Estados Unidos Fil: Stallard, Tom. University of Leicester; Reino Unido Fil: Tiscareno, Matthew S.. Cornell University; Estados Unidos Fil: Tobie, Gabriel. Centre de Recherche de Nantes; Francia Fil: Bacon, Andrew. Systems Engineering and Asssessment Ltd; Reino Unido Fil: Chaloner, Chris. Systems Engineering and Asssessment Ltd; Reino Unido Fil: Guest, Michael. Systems Engineering and Asssessment Ltd; Reino Unido Fil: Kemble, Steve. Astrium; Reino Unido Fil: Peacocke, Lisa. Astrium; Reino Unido Fil: Achilleos, Nicholas. University College London; Estados Unidos Fil: Andert, Thomas P.. Universität der Bundeswehr; Alemania Fil: Banfield, Don. Cornell University; Estados Unidos Fil: Barabash, Stas. Sweden Institute of Space Physics; Suecia Fil: Barthelemy, Matthieu. Universite Joseph Fourier; Francia Fil: Bertucci, Cesar. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; Argentina Fil: Brandt, Pontus. University Johns Hopkins; Estados Unidos Fil: Cecconi, Baptiste. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Chakrabarti, Supriya. Boston University; Estados Unidos

Published
2012

47. Solar wind pressure effects on Jupiter decametric radio emissions independent of Io

Author

Ezequiel Echer, Ph. Zarka, Sebastien Hess, HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Pesquisas Espaciais (INPE), Ministério da Ciência, Tecnologia e Inovação, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::High Energy Astrophysical Phenomena, Solar wind, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Atmospheric sciences, 01 natural sciences, 7. Clean energy, Jupiter magnetosphere, Jupiter, Interplanetary scintillation, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Bow shocks in astrophysics, 13. Climate action, Space and Planetary Science, Magnetosphere of Saturn, Physics::Space Physics, Magnetopause, Astrophysics::Earth and Planetary Astrophysics, Jupiter auroral radio emission, Magnetosphere of Jupiter, Decametric radio emission
Abstract

International audience; This paper investigates the effects of the solar wind dynamic pressure on Jupiter auroral radio emissions at decametric wavelengths that are not controlled by the electrodynamic interaction with the moon Io (non-Io DAM). In order to conduct this study, Nançay decametric array radio data are analyzed for the 1996-1999 period. Solar wind conditions at Jupiter's orbit are studied using the Michigan University solar wind propagation model (mSWiM). Interplanetary fast shocks (forward shocks, FS, or reverse shocks, RS), and average solar wind dynamic pressure are correlated with non-Io DAM emission occurrence, duration and power. It is found that non-Io DAM emissions occur preferentially during periods of enhanced solar wind dynamic pressure and after a FS or a RS arrival at Jupiter. The dawn (non-Io B-type) and dusk (non-Io-A-type) radio emissions are investigated separately and show (1) a dawn-dusk asymmetry consistent with prior studies and auroral ultraviolet (UV) observations, and (2) different behaviors in response to solar wind shocks. Our study confirms the solar wind control of - at least a part of - the non-Io DAM, and refines the scenario of response of the radio emissions to the solar wind interaction with the Jovian magnetosphere.

Published
2012

48. Longitudinal modulation of hot electrons in the Io plasma torus

Author

Sebastien Hess, Peter A. Delamere, Fran Bagenal, Andrew J. Steffl, and Nicholas M. Schneider

Subjects
Physics, Atmospheric Science, education.field_of_study, Ecology, Flux tube, Population, Paleontology, Soil Science, Flux, Forestry, Torus, Plasma, Aquatic Science, Oceanography, Magnetic field, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Modulation (music), Earth and Planetary Sciences (miscellaneous), Current (fluid), Atomic physics, education, Earth-Surface Processes, Water Science and Technology
Abstract

[1] The longitudinal modulation in the Io torus has been an open question for decades. A major clue was provided by the discovery of the key modulation of the hot electron population, at both the System III and System IV periods. However, very little progress has been made in explaining the origin of these hot electron modulations. We propose that the hot electrons population is powered by the inward motion of empty flux tubes (i.e. related to the outward transport of the Iogenic plasma), which has been observed in the torus. We propose that the System IV and System III modulation of the hot electron population corresponds to modulation of the intensity of the current system and of the efficiency of the electron acceleration, respectively. We build on the latest models of the Io current system to describe the current system associated with the motion of the empty flux tubes, and the associated electron acceleration. The System III modulation of the hot electron population, due to the modulation of the efficiency of the electron acceleration, can then be related to the topology of the magnetic field. We show through calculation and simulation that the electron acceleration related to the inward motion of the empty flux tube may explain the observations. We discuss the energy budget and show that it is in favor of our hypothesis.

Published
2011

49. Size and amplitude of Langmuir waves in the solar wind

Author

Robert E. Ergun, Sebastien Hess, and David M. Malaspina

Subjects
Atmospheric Science, Wave packet, Soil Science, Aquatic Science, Oceanography, Plasma oscillation, Kinetic energy, Optics, Geochemistry and Petrology, Normal mode, Earth and Planetary Sciences (miscellaneous), Earth-Surface Processes, Water Science and Technology, Physics, Ecology, business.industry, Turbulence, Paleontology, Forestry, Solar physics, Computational physics, Solar wind, Geophysics, Amplitude, Space and Planetary Science, Physics::Space Physics, business
Abstract

[1] Langmuir waves in the solar wind are known to be the origin of many types of solar radio emissions. In situ observations have shown that the most intense Langmuir waves often appear as wave packets. Several models have been proposed to explain this localization, such as kinetic localization and eigenmode formation. In the present paper we investigate the role of background turbulence on the size of the Langmuir wave packets through modeling of both quasi-planar growth in constant density regions and eigenmode growth in density wells. We compute both numerically and analytically the growth of the waves, the size of the wave packets, and the amplitude of these packets. Our theoretical results are compared to the in situ measurements of Ulysses and STEREO and appear to be consistent with the measured amplitude distributions.

Published
2011

50. Model of the Jovian magnetic field topology constrained by the Io auroral emissions

Author

Denis Grodent, Bertrand Bonfond, Sebastien Hess, and P. Zarka

Subjects
Atmospheric Science, Field line, Soil Science, Aquatic Science, Oceanography, Jovian, L-shell, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Mercury's magnetic field, Magnetosphere particle motion, Earth-Surface Processes, Water Science and Technology, Physics, Ecology, Paleontology, Forestry, Dipole model of the Earth's magnetic field, Geophysics, Computational physics, Earth's magnetic field, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Magnetosphere of Jupiter
Abstract

[1] The determination of the internal magnetic field of Jupiter has been the object of many studies and publications. These models have been computed from the Pioneer, Voyager, and Ulysses measurements. Some models also use the position of the Io footprints as a constraint: the magnetic field lines mapping to the footprints must have their origins along Io's orbit. The use of this latter constraint to determine the internal magnetic field models greatly improved the modeling of the auroral emissions, in particular the radio ones, which strongly depends on the magnetic field geometry. This constraint is, however, not sufficient for allowing a completely accurate modeling. The fact that the footprint field line should map to a longitude close to Io's was not used, so that the azimuthal component of the magnetic field could not be precisely constrained. Moreover, a recent study showed the presence of a magnetic anomaly in the northern hemisphere, which has never been included in any spherical harmonic decomposition of the internal magnetic field. We compute a decomposition of the Jovian internal magnetic field into spherical harmonics, which allows for a more accurate mapping of the magnetic field lines crossing Io, Europa, and Ganymede orbits to the satellite footprints observed in UV. This model, named VIPAL, is mostly constrained by the Io footprint positions, including the longitudinal constraint, and normalized by the Voyager and Pioneer magnetic field measurements. We show that the surface magnetic fields predicted by our model are more consistent with the observed frequencies of the Jovian radio emissions than those predicted by previous models.

Published
2011

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