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13 results on '"Solar-Terrestrial relations"'

1. Study of two interacting interplanetary coronal mass ejections encountered by Solar Orbiter during its first perihelion passage. Observations and modeling

Author

D. Telloni, C. Scolini, C. Möstl, G. P. Zank, L.-L. Zhao, A. J. Weiss, M. A. Reiss, R. Laker, D. Perrone, Y. Khotyaintsev, K. Steinvall, L. Sorriso-Valvo, T. S. Horbury, R. F. Wimmer-Schweingruber, R. Bruno, R. D’Amicis, R. De Marco, V. K. Jagarlamudi, F. Carbone, R. Marino, M. Stangalini, M. Nakanotani, L. Adhikari, H. Liang, L. D. Woodham, E. E. Davies, H. Hietala, S. Perri, R. Gómez-Herrero, J. Rodríguez-Pacheco, E. Antonucci, M. Romoli, S. Fineschi, M. Maksimovic, J. Souček, T. Chust, M. Kretzschmar, A. Vecchio, D. Müller, I. Zouganelis, R. M. Winslow, S. Giordano, S. Mancuso, R. Susino, S. L. Ivanovski, M. Messerotti, H. O’Brien, V. Evans, V. Angelini, École Centrale de Lyon (ECL), Université de Lyon, Centre National de la Recherche Scientifique (CNRS), and Commission of the European Communities

Subjects
010504 meteorology & atmospheric sciences, Sun: coronal mass ejections (CMEs), Astronomy, Astrophysics, Astronomy & Astrophysics, ACCELERATION, 7. Clean energy, 01 natural sciences, magnetohydrodynamics (MHD), law.invention, Orbiter, [SPI]Engineering Sciences [physics], MAGNETIC CLOUD EROSION, law, 0103 physical sciences, 0201 Astronomical and Space Sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, COMPLEX EJECTA, Sun: heliosphere, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], Science & Technology, Astronomy and Astrophysics, WIND, solar-terrestrial relations, ARRIVAL-TIME, EVOLUTION, Sun: evolution, solar wind, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physical Sciences, solar wind solar-terrestrial relations, Physics::Space Physics, SHOCK, TURBULENCE, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, FLUX ROPES, IN-SITU OBSERVATIONS
Abstract

Context. Solar Orbiter, the new-generation mission dedicated to solar and heliospheric exploration, was successfully launched on February 10, 2020, 04:03 UTC from Cape Canaveral. During its first perihelion passage in June 2020, two successive interplanetary coronal mass ejections (ICMEs), propagating along the heliospheric current sheet (HCS), impacted the spacecraft. Aims. This paper addresses the investigation of the ICMEs encountered by Solar Orbiter on June 7−8, 2020, from both an observational and a modeling perspective. The aim is to provide a full description of those events, their mutual interaction, and their coupling with the ambient solar wind and the HCS. Methods. Data acquired by the MAG magnetometer, the Energetic Particle Detector suite, and the Radio and Plasma Waves instrument are used to provide information on the ICMEs’ magnetic topology configuration, their magnetic connectivity to the Sun, and insights into the heliospheric plasma environment where they travel, respectively. On the modeling side, the Heliospheric Upwind eXtrapolation model, the 3D COronal Rope Ejection technique, and the EUropean Heliospheric FORecasting Information Asset (EUHFORIA) tool are used to complement Solar Orbiter observations of the ambient solar wind and ICMEs, and to simulate the evolution and interaction of the ejecta in the inner heliosphere, respectively. Results. Both data analysis and numerical simulations indicate that the passage of two distinct, dynamically and magnetically interacting (via magnetic reconnection processes) ICMEs at Solar Orbiter is a possible scenario, supported by the numerous similarities between EUHFORIA time series at Solar Orbiter and Solar Orbiter data. Conclusions. The combination of in situ measurements and numerical simulations (together with remote sensing observations of the corona and inner heliosphere) will significantly lead to a deeper understanding of the physical processes occurring during the CME-CME interaction.

Published
2021

2. Characteristics and Energy Dependence of Recurrent Galactic Cosmic-Ray Flux Depressions and of a Forbush Decrease with LISA Pathfinder

Author

C. Zenoni, Lluis Gesa, J. Martino, A. Zambotti, Gerhard Heinzel, R. Maarschalkerweerd, A. Wittchen, I. Harrison, L. Martin-Polo, N. Korsakova, Stefano Vitale, Luis Mendes, J. A. Lobo, Marco Freschi, Nikolaos Karnesis, Jacob Slutsky, Valerio Ferroni, B. Kaune, D. Hoyland, Antoine Petiteau, L. Wissel, Daniele Bortoluzzi, Paul McNamara, T. J. Sumner, L. Liu, Pierre Binétruy, Carlos F. Sopuerta, Catia Grimani, Antonella Cavalleri, Ignacio Mateos, Heather Audley, Daniele Vetrugno, Miquel Nofrarías, J. Baird, Massimo Bassan, Monica Laurenza, Davor Mance, M. Born, Federico Sabbatini, F. Martin-Porqueras, James Ira Thorpe, Michele Armano, A. M. Cruise, Philippe Jetzer, E. D. Fitzsimons, Christian J. Killow, Karsten Danzmann, J. Grzymisch, H. Ward, J. Reiche, P. Pivato, D. I. Robertson, Henri Inchauspe, Ingo Diepholz, A. Cesarini, G. Russano, M. Fabi, M. de Deus Silva, Mauro Hueller, R. Giusteri, G. Dixon, Peter Wass, S. Paczkowski, N. Finetti, F. Rivas, Peter Zweifel, Rita Dolesi, Oliver Jennrich, Eric Plagnol, Michael Perreur-Lloyd, Gudrun Wanner, Domenico Giardini, Juan Ramos-Castro, Vicente Martín, Daniel Hollington, Simone Benella, Daniele Telloni, Ivan Lloro, J. P. López-Zaragoza, Ferran Gibert, Damien Texier, Luigi Ferraioli, José F. F. Mendes, M. Hewitson, W. J. Weber, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universitat Politècnica de Catalunya. Departament d'Enginyeria Electrònica, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Astrofísica, solar–terrestrial relations, 010504 meteorology & atmospheric sciences, 0306 Physical Chemistry (Incl. Structural), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], interferometers [instrumentation], Astrophysics, 01 natural sciences, 0305 Organic Chemistry, 27-DAY VARIATION, Physics - Space Physics, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, cosmic rays, instrumentation: interferometers, interplanetary medium, solar-terrestrial relations, Sun: heliosphere, Sun: rotation, 010303 astronomy & astrophysics, Sun rotation, Solar–terrestrial relations, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), heliosphere [Sun], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Space physics, charged particle, solar, ELECTRONS, CORONAL MASS EJECTIONS, interferometers, Sun: rotation [cosmic rays, instrumentation], Astrophysics - Solar and Stellar Astrophysics, SOLAR-WIND, cosmic radiation: galaxy, Physical Sciences, Physics::Space Physics, Solar rotation, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, cosmic radiation: flux, Astrophysics::High Energy Astrophysical Phenomena, HELIOSPHERIC MODULATION, Interplanetary medium, FOS: Physical sciences, Cosmic ray, rotation [Sun], Astronomy & Astrophysics, 0103 physical sciences, PARTICLES, Forbush decrease, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], instrumentation interferometers, SPACED DATA, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Sun heliosphere, solar terrestrial relations, SPECTRUM, LISA, Science & Technology, cosmic radiation: energy spectrum, INTENSITY, POSITRONS, Astronomy and Astrophysics, Space Physics (physics.space-ph), cosmic rays, instrumentation interferometers, interplanetary medium, solar terrestrial relations, Sun heliosphere, Sun rotation, 0201 Astronomical And Space Sciences, monitoring, 13. Climate action, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], charged particle: detector, Interplanetary spaceflight, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere
Abstract

The final publication is available at IOS Press through http://dx.doi.org/10.3847/1538-4357/aaa774 Galactic cosmic-ray (GCR) energy spectra observed in the inner heliosphere are modulated by the solar activity, the solar polarity and structures of solar and interplanetary origin. A high counting rate particle detector (PD) aboard LISA Pathfinder, meant for subsystems diagnostics, was devoted to the measurement of GCR and solar energetic particle integral fluxes above 70 MeV n-1 up to 6500 counts s-1. PD data were gathered with a sampling time of 15 s. Characteristics and energy dependence of GCR flux recurrent depressions and of a Forbush decrease dated 2016 August 2 are reported here. The capability of interplanetary missions, carrying PDs for instrument performance purposes, in monitoring the passage of interplanetary coronal mass ejections is also discussed.

Published
2018

3. Solar radio bursts as a tool for space weather forecasting

Author

Klein, Karl-Ludwig, Salas Matamoros, Carolina, Zucca, Pietro, 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), Université Paris sciences et lettres (PSL), ANR-14-ASTR-0027,ORME,Outils radio astronomiques pour la météorologie de l'espace(2014), European Project: 637324,H2020,H2020-PROTEC-2014,HESPERIA(2015), 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 Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL), 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), and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)

Subjects
Sun: coronal mass ejection, Sun: radio radiation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Sun: particle emission, Soleil : émission de particules, Soleil : émissions radio, Soleil : éjection coronale de masse, Relations Soleil-Terre, Solar–terrestrial relations, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
Abstract

International audience; The solar corona and its activity induce disturbances that may affect the space environment of the Earth. Noticeable disturbances come from coronal mass ejections (CMEs), which are large-scale ejections of plasma and magnetic fields from the solar corona, and solar energetic particles (SEPs). These particles are accelerated during the explosive variation of the coronal magnetic field or at the shock wave driven by a fast CME. In this contribution, it is illustrated how full Sun microwave observations can lead to (1) an estimate of CME speeds and of the arrival time of the CME at the Earth, (2) the prediction of SEP events attaining the Earth.; La couronne solaire et son activité peuvent perturber l'environnement spatial de la Terre. Les éjections coronales de masse (CME) sont des instabilités à grande échelle qui conduisent à l'éjection dans l'espace interplanétaire du plasma et du champ magnétique qui le confine. D'autres perturbations viennent des particules solaires de haute énergie (SEP). Elles sont accélérées au cours de la variation explosive du champ magnétique ou par l'onde de choc qu'engendre une CME rapide. Dans cet article, on illustre comment des observations du Soleil entier en micro-ondes peuvent conduire (1) à estimer la vitesse d'une CME et son temps d'arrivée à la Terre, (2) à la prévision des événements solaires à particules qui atteignent la Terre.

Published
2018

4. Exploring the potential of microwave diagnostics in SEP forecasting: The occurrence of SEP events

Author

Pietro Zucca, Karl-Ludwig Klein, Marlon Núñez, Netherlands Institute for Radio Astronomy (ASTRON), 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
Atmospheric Science, 010504 meteorology & atmospheric sciences, Meteorology, lcsh:QC851-999, 01 natural sciences, Sun: particle emission, 0103 physical sciences, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Remote sensing, Spacecraft, Solar energetic particles, Sun: radio radiation, business.industry, Geosynchronous orbit, Solar telescope, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Solar-terrestrial relations, Geostationary orbit, Solar particle event, Environmental science, lcsh:Meteorology. Climatology, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Microwave, Space environment
Abstract

Solar energetic particles (SEPs), especially protons and heavy ions, may be a space-weather hazard when they impact spacecraft and the terrestrial atmosphere. Forecasting schemes have been developed, which use earlier signatures of particle acceleration to predict the arrival of solar protons and ions in the space environment of the Earth. The UMASEP (University of MAlaga Solar particle Event Predictor) scheme forecasts the occurrence and the importance of an SEP event based on combined observations of soft X-rays, their time derivative and protons above 10 MeV at geosynchronous orbit. We explore the possibility to replace the derivative of the soft X-ray time history with the microwave time history in the UMASEP scheme. To this end we construct a continuous time series of observations for a 13-month period from December 2011 to December 2012 at two microwave frequencies, 4.995 and 8.8 GHz, using data from the four Radio Solar Telescope Network (RSTN) patrol stations of the US Air Force, and feed this time series to the UMASEP prediction scheme. During the selected period the Geostationary Operational Environmental Satellites (GOES) detected nine SEP events related to activity in the western solar hemisphere. We show that the SEP forecasting using microwaves has the same probability of detection as the method using soft X-rays, but no false alarm in the considered period, and a slightly increased warning time. A detailed analysis of the missed events is presented. We conclude that microwave patrol observations improve SEP forecasting schemes that employ soft X-rays. High-quality microwave data available in real time appear as a significant addition to our ability to predict SEP occurrence.

Published
2017

5. Quantitative model for the generic 3D shape of ICMEs at 1 AU

Author

Sergio Dasso, Miho Janvier, J. J. Masías-Meza, Pascal Démoulin, Université de Liège, 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), and EADS Astrium SAS

Subjects
010504 meteorology & atmospheric sciences, Ciencias Físicas, FOS: Physical sciences, Astrophysics, Space weather, 01 natural sciences, purl.org/becyt/ford/1 [https], HELIOSPHERE [SUN], 0103 physical sciences, Coronal mass ejection, SOLAR-TERRESTRIAL RELATIONS, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, [PHYS]Physics [physics], COSMIC cancer database, Spacecraft, business.industry, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], CORONAL MASS EJECTIONS (CMES) [SUN], MAGNETIC FIELDS [SUN], Computational physics, Astronomía, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physics::Space Physics, Plasma parameter, Impact parameter, business, Interplanetary spaceflight, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CIENCIAS NATURALES Y EXACTAS, Rope
Abstract

Interplanetary imagers provide 2D projected views of the densest plasma parts of interplanetary coronal mass ejections (ICMEs) while in situ measurements provide magnetic field and plasma parameter measurements along the spacecraft trajectory, so along a 1D cut. As such, the data only give a partial view of their 3D structures. By studying a large number of ICMEs, crossed at different distances from their apex, we develop statistical methods to obtain a quantitative generic 3D shape of ICMEs. In a first approach we theoretically obtain the expected statistical distribution of the shock-normal orientation from assuming simple models of 3D shock shapes, including distorted profiles, and compare their compatibility with observed distributions. In a second approach we use the shock normal and the flux rope axis orientations, as well as the impact parameter, to provide statistical information across the spacecraft trajectory. The study of different 3D shock models shows that the observations are compatible with a shock symmetric around the Sun-apex line as well as with an asymmetry up to an aspect ratio around 3. Moreover, flat or dipped shock surfaces near their apex can only be rare cases. Next, the sheath thickness and the ICME velocity have no global trend along the ICME front. Finally, regrouping all these new results and the ones of our previous articles, we provide a quantitative ICME generic 3D shape, including the global shape of the shock, the sheath and the flux rope. The obtained quantitative generic ICME shape will have implications for several aims. For example, it constrains the output of typical ICME numerical simulations. It is also a base to develop deeper studies of the transport of high energy solar and cosmic particles during an ICME propagation, as well as for modeling and forecasting space weather conditions near Earth., 14 pages, 13 figures

Published
2016

6. Coronal mass ejection-related particle acceleration regions during a simple eruptive event

Author

Alexis P. Rouillard, Carolina Salas-Matamoros, Karl-Ludwig Klein, 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), Space Research Center [Costa Rica], Universidad Nacional de Costa Rica, Unité Scientifique de la Station de Nançay (USN), 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), 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)-Université d'Orléans (UO), 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), ANR-14-ASTR-0027,ORME,Outils radio astronomiques pour la météorologie de l'espace(2014), European Project: 606692,EC:FP7:SPA,FP7-SPACE-2013-1,HELCATS(2014), 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 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), and 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)

Subjects
Sun: flares, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Coronal hole, Astrophysics, 01 natural sciences, Sun: particle emission, 0103 physical sciences, Sun: coronal mass ejections (CMEs, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Interplanetary magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, acceleration of particles, Physics, Solar flare, Sun: radio radiation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy, Astronomy and Astrophysics, solar-terrestrial relations, Corona, Nanoflares, Solar wind, Space and Planetary Science, Physics::Space Physics, Heliosphere
Abstract

International audience; An intriguing feature of many solar energetic particle (SEP) events is the detection of particles over a very extended range of longitudes in the heliosphere. This may be due to peculiarities of the magnetic field in the corona, to a broad accelerator, to cross-field transport of the particles, or to a combination of these processes. The eruptive flare on 26 April 2008 provided an opportunity to study relevant processes under particularly favourable conditions since it occurred in a very quiet solar and interplanetary environment. This enabled us to investigate the physical link between a single well-identified coronal mass ejection (CME), electron acceleration as traced by radio emission, and the production of SEPs. We conduct a detailed analysis, which combines radio observations (Nançay Radio Heliograph and Nançay Decametre Array, Wind/Waves spectrograph) with remote-sensing observations of the corona in extreme ultraviolet (EUV) and white light, as well as in situ measurements of energetic particles near 1AU (SoHO and STEREO spacecraft). By combining images taken from multiple vantage points, we were able to derive the time-dependent evolution of the 3D pressure front that was developing around the erupting CME. Magnetic reconnection in the post-CME current sheet accelerated electrons, which remained confined in closed magnetic fields in the corona, while the acceleration of escaping particles can be attributed to the pressure front ahead of the expanding CME. The CME accelerated electrons remotely from the parent active region, owing to the interaction of its laterally expanding flank, which was traced by an EUV wave, with the ambient corona. SEPs detected at one STEREO spacecraft and SoHO were accelerated later, when the frontal shock of the CME intercepted the spacecraft-connected interplanetary magnetic field line. The injection regions into the heliosphere inferred from the radio and SEP observations are separated in longitude by about 140 •. The observations for this event show that it is misleading to interpret multi-spacecraft SEP measurements in terms of one acceleration region in the corona. The different acceleration regions are linked to different vantage points in the interplanetary space.

Published
2016

7. Segmentation of coronal features to understand the solar EUV and UV irradiance variability

Author

Joe Zender, Cis Verbeeck, Lakshmi Pradeep Chitta, Luc Damé, Gabriel Giono, R. Kariyappa, Véronique Delouille, Vijayakumar H. Doddamani, S. T. Kumara, B. Mampaey, Jean-François Hochedez, APS College of Engineering, Indian Institute of Astrophysics (IIA), Department of physics [BU Bangalore], Bangalore University, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), National Astronomical Observatory of Japan (NAOJ), Royal Observatory of Belgium [Brussels] (ROB), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, 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), European Space Agency (ESA), and Smithsonian Institution-Harvard University [Cambridge]

Subjects
010504 meteorology & atmospheric sciences, Extreme ultraviolet lithography, Irradiance, Coronal hole, Context (language use), Space weather, Solar irradiance, 7. Clean energy, 01 natural sciences, Heliophysics, Sun: activity, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Physics, Radiometer, Sun: corona, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Sun: UV radiation, Sun: evolution, 13. Climate action, Space and Planetary Science, Solar-terrestrial relations, Sun: atmosphere
Abstract

International audience; Context. The study of solar irradiance variability is of great importance in heliophysics, the Earth’s climate, and space weather applications. These studies require careful identifying, tracking and monitoring of active regions (ARs), coronal holes (CHs), and the quiet Sun (QS).Aims. We studied the variability of solar irradiance for a period of two years (January 2011–December 2012) using the Large Yield Radiometer (LYRA), the Sun Watcher using APS and image Processing (SWAP) on board PROBA2, and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO).Methods. We used the spatial possibilistic clustering algorithm (SPoCA) to identify and segment coronal features from the EUV observations of AIA. The AIA segmentation maps were then applied on SWAP images, and parameters such as the intensity, fractional area, and contribution of ARs/CHs/QS features were computed and compared with the full-disk integrated intensity and LYRA irradiance measurements.Results. We report the results obtained from SDO/AIA and PROBA2/SWAP images taken from January 2011 to December 2012 and compare the resulting integrated full-disk intensity with PROBA2/LYRA irradiance. We determine the contributions of the segmented features to EUV and UV irradiance variations. The variations of the parameters resulting from the segmentation, namely the area, integrated intensity, and relative contribution to the solar irradiance, are compared with LYRA irradiance. We find that the active regions have a great impact on the irradiance fluctuations. In the EUV passbands considered in this study, the QS is the greatest contributor to the solar irradiance, with up to 63% of total intensity values. Active regions, on the other hand, contribute to about 10%, and off-limb structures to about 24%. We also find that the area of the features is highly variable suggesting that their area has to be taken into account in irradiance models, in addition to their intensity variations.Conclusions. We successfully show that the feature extraction allows us to use EUV telescopes to measure irradiance fluctuations and to quantify the contribution of each part to the EUV spectral solar irradiance observed with a calibrated radiometer. This study also shows that SPoCA is viable, and that the segmentation of images can be a useful tool. We also provide the measurement correlation between SWAP and AIA during this analysis.

Published
2014

8. No evidence for planetary influence on solar activity 330 000 years ago

Author

Grant M. Raisbeck, Jean Jouzel, Edouard Bard, Alexandre Cauquoin, Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Glaces et Continents, Climats et Isotopes Stables (GLACCIOS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-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], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Context (language use), Tachocline, Astrophysics, 01 natural sciences, Astrobiology, Ice core, Sun: activity, 0103 physical sciences, planet-star interactions, Cosmogenic nuclide, 010303 astronomy & astrophysics, Sun: magnetic fields, Holocene, 0105 earth and related environmental sciences, Physics, Sunspot, sunspots, Astronomy and Astrophysics, dynamo, solar-terrestrial relations, Solar cycle, 13. Climate action, Space and Planetary Science, Climatology, Interglacial
Abstract

Context. Abreu et al. (2012, A&A. 548, A88) have recently compared the periodicities in a 14 C – 10 Be proxy record of solar variability during the Holocene and found a strong similarity with the periodicities predicted on the basis of a model of the time-dependent torque exerted by the planets on the sun’s tachocline. If verified, this effect would represent a dramatic advance not only in the basic understanding of the Sun’s variable activity, but also in the potential influence of this variability on the Earth’s climate. Cameron and Schussler (2013, A&A. 557, A83) have seriously criticized the statistical treatment used by Abreu et al. to test the significance of the coincidences between the periodicities of their model with the Holocene proxy record.Aims. If the Abreu et al. hypothesis is correct, it should be possible to find the same periodicities in the records of cosmogenic nuclides at earlier times.Methods. We present here a high-resolution record of 10 Be in the EPICA Dome C (EDC) ice core from Antarctica during the Marine Interglacial Stage 9.3 (MIS 9.3), 325–336 kyr ago, and investigate its spectral properties.Results. We find very limited similarity with the periodicities seen in the proxy record of solar variability during the Holocene, or with that of the model of Abreu et al.Conclusions. We find no support for the hypothesis of a planetary influence on solar activity, and raise the question of whether the centennial periodicities of solar activity observed during the Holocene are representative of solar activity variability in general.

Published
2014

9. Does spacecraft trajectory strongly affect detection of magnetic clouds?

Author

Pascal Démoulin, Miho Janvier, Sergio Dasso, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, 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), Instituto de Astronomía y Física del Espacio [Buenos Aires] (IAFE), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET)-Universidad de Buenos Aires [Buenos Aires] (UBA), service hématologie Nantes, and Centre hospitalier universitaire de Nantes (CHU Nantes)

Subjects
Uniform distribution (continuous), 010504 meteorology & atmospheric sciences, Ciencias Físicas, Uniform distribution, Flux, Astrophysics, Parameter space, 01 natural sciences, Planetary surface analysis, Trajectories, purl.org/becyt/ford/1 [https], Magnetic flux ropes, Parameter spaces, Rotation angles, Current distribution, Natural consequences, coronal mass ejection [Sun], Spacecraft, 010303 astronomy & astrophysics, Magnetic flux, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], heliosphere [Sun], Computer simulation, Aspect ratio, Solar wind, Physics::Space Physics, Magnetic clouds, Impact parameter, CIENCIAS NATURALES Y EXACTAS, Boundary shapes, Impact-parameter, Context (language use), Flux rope model, 0103 physical sciences, Force free fields, Parameter estimation, 0105 earth and related environmental sciences, Spacecraft trajectories, Affect detection, Decreasing functions, Flux ropes, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], coronal mass ejections (CMEs) [Sun], Frequency distributions, Computational physics, Astronomía, Low field, Space and Planetary Science, Magnetic fields, Solar-terrestrial relations, Large parts, Non-detection, Interplanetary coronal mass ejections, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliospheres, Rope
Abstract

Context. Magnetic clouds (MCs) are a subset of interplanetary coronal mass ejections (ICMEs). One property of MCs is the presence of a magnetic flux rope. Is the difference between ICMEs with and without MCs intrinsic or rather due to an observational bias? Aims. As the spacecraft has no relationship with the MC trajectory, the frequency distribution of MCs versus the spacecraft distance to the MCs’ axis is expected to be approximately flat. However, Lepping & Wu (2010, Ann. Geophys., 28, 1539) confirmed that it is a strongly decreasing function of the estimated impact parameter. Is a flux rope more frequently undetected for larger impact parameter? Methods. In order to answer the questions above, we explore the parameter space of flux rope models, especially the aspect ratio, boundary shape, and current distribution. The proposed models are analyzed as MCs by fitting a circular linear force-free field to the magnetic field computed along simulated crossings. Results. We find that the distribution of the twist within the flux rope and the non-detection due to too low field rotation angle or magnitude only weakly affect the expected frequency distribution of MCs versus impact parameter. However, the estimated impact parameter is increasingly biased to lower values as the flux rope cross section is more elongated orthogonally to the crossing trajectory. The observed distribution of MCs is a natural consequence of a flux rope cross section flattened on average by a factor 2 to 3 depending on the magnetic twist profile. However, the faster MCs at 1 AU, with V > 550 km s-1, present an almost uniform distribution of MCs vs. impact parameter, which is consistent with round-shaped flux ropes, in contrast with the slower ones. Conclusions. We conclude that the sampling of MCs at various distances from the axis does not significantly affect their detection. The large part of ICMEs without MCs could be due to a too strict criteria for MCs or to the fact that these ICMEs are encountered outside their flux rope or near the leg region, or they do not contain a flux rope. Fil: Démoulin, Pascal. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia Fil: Dasso, Sergio Ricardo. 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: Janvier, M.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia

Published
2013

10. Prototyping a global soft X-ray imaging instrument for heliophysics, planetary science, and astrophysics science

Author

Collier, Michael R., Porter, Frederick S., Sibeck, David G., Carter, Jenny A., Chiao, Meng P., Chornay, Dj., Cravens, T., Galeazzi, Massimiliano, Keller, John W., Koutroumpa, Dimitra, Kuntz, K., Read, A. M., Robertson, I. P., Sembay, S., Snowden, S., Thomas, N., NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Leicester], University of Leicester, Department of Physics and Astronomy [Lawrence Kansas], University of Kansas [Lawrence] (KU), Department of Physics [Coral Gables], University of Miami [Coral Gables], 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), Department of Physics and Astronomy [Baltimore], and Johns Hopkins University (JHU)

Subjects
[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Solar wind, Physics::Space Physics, Solar-terrestrial relations, Astrophysics::Instrumentation and Methods for Astrophysics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Earth and Planetary Astrophysics, X-rays: diffuse background, Interplanetary medium
Abstract

International audience; We describe current progress in the development of a prototype wide field-of-view soft X-ray imager that employs Lobster-eye optics and targets heliophysics, planetary, and astrophysics science. The prototype will provide proof-of-concept for a future flight instrument capable of imaging the entire dayside magnetosheath from outside the magnetosphere. Such an instrument was proposed for the ESA AXIOM mission

Published
2012

11. The Sun as a star: observations of white-light flares

Author

Matthieu Kretzschmar, 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), European Project: 218816,EC:FP7:SPA,FP7-SPACE-2007-1,SOTERIA(2008), and Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Spectral power distribution, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), Irradiance, FOS: Physical sciences, Context (language use), Astrophysics, sun: flares, Solar irradiance, 01 natural sciences, 7. Clean energy, law.invention, law, Sun: activity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Solar flare, Astronomy and Astrophysics, solar-terrestrial relations, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, stars: flare, Astrophysics - Earth and Planetary Astrophysics, Flare
Abstract

International audience; Context. Solar flares radiate energy at all wavelengths, but the spectral distribution of this energy is still poorly known. White-light continuum emission is sometimes observed, and these flares are then called " white-light flares " (WLFs). Aims. We investigate if all flares are WLFs and how the radiated energy is distributed spectrally. Methods. We perform a superposed epoch analysis of spectral and total irradiance measurements obtained since 1996 by the SOHO and GOES spacecraft at various wavelengths, from soft X-rays to the visible domain. Results. The long-term record of solar irradiance and the excellent duty cycle of the measurements allow us to detect a signal in visible irradiance even for moderate (C-class) flares mainly during the impulsive phase. We identify this signal as continuum emission emitted by WLFs and find that it is consistent with a blackbody emission at ∼9000 K. We estimate the contribution of the WL continuum for several sets of flares and find it to be about 70% of the total radiated energy. We re-analyse the X17 flare that occurred on 28 October 2003 and find similar results. Conclusions. We show that most of the flares – if not all – are WLFs and that the white-light continuum is the main contributor to the total radiated energy; this continuum is consistent with a blackbody spectrum at ∼9000 K. These observational results are important for understanding the physical mechanisms during flares and possibly suggest a contribution of flares to the variations of the total solar irradiance (TSI).

Published
2011

12. Mars environment and magnetic orbiter model payload

Author

J.E. Walhund, A. Pais, Pascal Tarits, S. Barabash, François Leblanc, T. Ott, Mioara Mandea, Stephen R. Lewis, Benoit Langlais, Helmut Lammer, Jean-Gabriel Trotignon, Eric Chassefière, J.G.M. Merayo, Martin Paetzold, Peter L. Read, Henri Rème, Gabriele Cremonese, François Forget, Andrew J. Coates, Susanne Vennerstrøm, Christophe Sotin, Michel Menvielle, Véronique Dehant, Miguel Lopez-Valverde, Doris Breuer, T. Fouchet, Graziella Branduardi-Raymont, 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), PLANETO - 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 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), Swedish Institute of Space Physics [Uppsala] (IRF), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Royal Observatory of Belgium [Brussels] (ROB), 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), GeoForschungsZentrum - Helmholtz-Zentrum Potsdam (GFZ), HELIOS - LATMOS, Department of Physics [Coimbra], University of Coimbra [Portugal] (UC), Universität zu Köln, Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], Institut Universitaire Européen de la Mer (IUEM), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Swedish Space Corporation (SSC), Centre d'étude spatiale des rayonnements (CESR), 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, 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), 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 ), IMPEC - 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 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 ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] ( DLR ), 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 ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Royal Observatory of Belgium [Brussels], 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 Paris ) -École normale supérieure - Paris ( ENS Paris ), Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), The Open University [Milton Keynes] ( OU ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), GeoForschungsZentrum - Helmholtz-Zentrum Potsdam ( GFZ ), HEPPI - LATMOS, University of Coimbra [Portugal] ( UC ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Institut Universitaire Européen de la Mer ( IUEM ), Institut de Recherche pour le Développement ( IRD ) -Université de Brest ( UBO ) -Centre National de la Recherche Scientifique ( CNRS ), National Space Institute [Lyngby] ( DTU Space ), Technical University of Denmark [Lyngby] ( DTU ), INAF - Osservatorio Astronomico di Padova ( OAPD ), Istituto Nazionale di Astrofisica ( INAF ), Swedish Space Corporation ( SSC ), 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 ), 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 ), 2.3 Earth's Magnetic Field, 2.0 Physics of the Earth, Departments, GFZ Publication Database, Deutsches GeoForschungsZentrum, 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), Universität zu Köln = University of Cologne, University of Oxford, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), 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), and Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Solar System, Cosmic Vision, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], planetary interior, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 550 - Earth sciences, 01 natural sciences, 7. Clean energy, law.invention, Atmosphere, Orbiter, law, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Orbital elements, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Space vehicles, Mars Exploration Program, M-class mission, planetary evolution, solar conditions, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Solar wind, [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], 13. Climate action, Space and Planetary Science, MEMO, Magnetic fields, atmosphere, Physics::Space Physics, Solar-terrestrial relations, Mars Environment and Magnetic Orbiter, Timekeeping on Mars, Astrophysics::Earth and Planetary Astrophysics, Planets and satellites, Solar system
Abstract

International audience; Mars Environment and Magnetic Orbiter was proposed as an answer to the Cosmic Vision Call of Opportunity as a M-class mission. The MEMO mission is designed to study the strong interconnections between the planetary interior, atmosphere and solar conditions essential to understand planetary evolution, the appearance of life and its sustainability. MEMO provides a high-resolution, complete, mapping of the magnetic field (below an altitude of about 250 km), with an yet unachieved full global coverage. This is combined with an in situ characterization of the high atmosphere and remote sensing of the middle and lower atmospheres, with an unmatched accuracy. These measurements are completed by an improved detection of the gravity field signatures associated with carbon dioxide cycle and to the tidal deformation. In addition the solar wind, solar EUV/UV and energetic particle fluxes are simultaneously and continuously monitored. The challenging scientific objectives of the MEMO mission proposal are fulfilled with the appropriate scientific instruments and orbit strategy. MEMO is composed of a main platform, placed on a elliptical (130 × 1,000 km), non polar (77° inclination) orbit, and of an independent, higher apoapsis (10,000 km) and low periapsis (300 km) micro-satellite. These orbital parameters are designed so that the scientific return of MEMO is maximized, in terms of measurement altitude, local time, season and geographical coverage. MEMO carry several suites of instruments, made of an ‘exospheric-upper atmosphere’ package, a ‘magnetic field’ package, and a ‘low-middle atmosphere’ package. Nominal mission duration is one Martian year.

Published
2009

13. A Terrella Device for Simulating Aurora-Like Phenomena in a Box

Author

Mauro Messerotti, R. Baccomi, D. Iugovaz, Jean Lilensten, INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Department of Physics, University of Trieste, Division of Trieste, National Institute for Nuclear Physics, Laboratoire de Planétologie de Grenoble (LPG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and the Italian Space Agency (ASI), the Italian National Institute for Astrophysics (INAF), the Trieste Division of the Italian National Institute for Nuclear Physics (INFN) and the Department of Physics of the Trieste University

Subjects
Physics, Terrella, Aurora, Meteorology, Bar (music), business.industry, Astronomy and Astrophysics, Space weather, 01 natural sciences, International Heliophysical Year, Magnetic field, Heliosphere, Space and Planetary Science, Magnet, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Vacuum chamber, Aerospace engineering, 010306 general physics, business, 010303 astronomy & astrophysics, Solar–terrestrial relations
Abstract

International audience; A Terrella device was developed and setup in Trieste in 2006 to be used as an experimental training device during practicum sessions of the Advanced International School on Space Weather at ICTP. The Terrella consisted of a vacuum chamber, where an aluminum sphere with an embedded permanent magnet bar mimics the Earth (Terrella) and its magnetic field, and a system of electrodes is set to a high potential difference to generate an electron flow (particle wind) that ionizes the residual air around the sphere. This results in aurora-like glowing patterns whose geometry is dependent on the orientation and distance of the bar magnet, so that various configurations can be experimented. This Terrella device proved to be an effective tool not only for academic but also for outreach purposes. We will briefly present both applications, focusing in particular on the latter, and on the planned use for IHY EPO activities.

Published
2009

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