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1. The Space Weather and Ultraviolet Solar Variability (SWUSV) Microsatellite Mission

Author: Luc Damé, Mustapha Meftah, Alain Hauchecorne, Philippe Keckhut, Alain Sarkissian, Marion Marchand, Abdenour Irbah, Éric Quémerais, Slimane Bekki, Thomas Foujols, Matthieu Kretzschmar, Gaël Cessateur, Alexander Shapiro, Werner Schmutz, Sergey Kuzin, Vladimir Slemzin, Alexander Urnov, Sergey Bogachev, José Merayo, Peter Brauer, Kanaris Tsinganos, Antonis Paschalis, Ayman Mahrous, Safinaz Khaled, Ahmed Ghitas, Besheir Marzouk, Amal Zaki, Ahmed A. Hady, and Rangaiah Kariyappa
Subjects: Solar eruptions, Coronal mass ejections, Space weather, Ultraviolet variability, Ultraviolet instrumentation, Solar irradiance, Medicine (General), R5-920, Science (General), Q1-390
Abstract: We present the ambitions of the SWUSV (Space Weather and Ultraviolet Solar Variability) Microsatellite Mission that encompasses three major scientific objectives: (1) Space Weather including the prediction and detection of major eruptions and coronal mass ejections (Lyman-Alpha and Herzberg continuum imaging); (2) solar forcing on the climate through radiation and their interactions with the local stratosphere (UV spectral irradiance from 180 to 400 nm by bands of 20 nm, plus Lyman-Alpha and the CN bandhead); (3) simultaneous radiative budget of the Earth, UV to IR, with an accuracy better than 1% in differential. The paper briefly outlines the mission and describes the five proposed instruments of the model payload: SUAVE (Solar Ultraviolet Advanced Variability Experiment), an optimized telescope for FUV (Lyman-Alpha) and MUV (200–220 nm Herzberg continuum) imaging (sources of variability); UPR (Ultraviolet Passband Radiometers), with 64 UV filter radiometers; a vector magnetometer; thermal plasma measurements and Langmuir probes; and a total and spectral solar irradiance and Earth radiative budget ensemble (SERB, Solar irradiance & Earth Radiative Budget). SWUSV is proposed as a small mission to CNES and to ESA for a possible flight as early as 2017–2018.
Published: 2013
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2. A detailed analysis of ion-acoustic waves observed in the solar wind by the Solar Orbiter

Author: David Pisa, Jan Soucek, Ondrej Santolik, Tomas Formanek, Milan Maksimovic, Thomas Chust, Yuri Khotyaintsev, Matthieu Kretzschmar, Christopher Owen, Philippe Louarn, and Andrei Fedorov
Abstract: Ion-acoustic waves are often observed in the solar wind along the Solar Orbiter’s orbit. These electrostatic waves are generated via ion-ion or current-driven instabilities below the local proton plasma frequency. Due to the Doppler shift, they are typically observed in the frequency range between the local electron and proton plasma frequency in the spacecraft frame. Ion-acoustic waves often accompany large-scale solar wind structures and play a role in the energy dissipation in the propagating solar wind. Time Domain Sampler (TDS) receiver, a part of the Radio and Plasma Waves (RPW) instrument, is sampling wave emissions at frequencies below 200 kHz almost continuously from the beginning of the mission. Almost three years of observations allow us to perform a detailed study of ion-acoustic waves in the solar wind under variable plasma conditions. The emission tends to be observed when proton density and temperature are highly perturbed. A detailed analysis of the proton velocity distribution and wave generation using solar wind data from a Proton and Alpha particle Sensor (PAS) of the Solar Wind Analyzer (SWA) is shown.
Published: 2023

3. An Empirical Model of the Variation of the Solar Lyman‐α Spectral Irradiance

Author: Matthieu Kretzschmar, Martin Snow, and Werner Curdt
Published: 2018
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4. Multispectral imaging the sun in the ultraviolet.

Author: Thierry Dudok De Wit, Saïd Moussaoui, Pierre-Olivier Amblard, Jean Aboudarham, Frederic Auchère, Matthieu Kretzschmar, and Jean Lilensten
Published: 2009
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5. What is the role of oblique whistler waves in shaping of the solar wind electron function between 0.17 and 1 AU ?

Author: Lucas Colomban, Matthieu Kretzschmar, Vladimir Krasnoselskikh, Milan Maksimovic, Daniel Graham, Yuri Khotyainsev, Laura Berĉiĉ, Matthieu Berthomier, and Clara Froment
Subjects: Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract: In the solar wind, whistler waves are thought to play an important role on the evolution of the electron velocity distribution function as a function of distance. In particular, oblique whistler waves may diffuse the Strahl electrons into the halo population. Using AC magnetic and electric field measured by the SCM (search coil magnetometer) and electric antenna of Solar Orbiter and Parker Solar Probe, we search for the presence of whistler waves at heliocentric distance between 0.17 and 1 AU. Spectral matrices computation and minimum variance analysis on continuous waveforms make it possible to identify whistler wave modes and to determine their direction of propagation with respect to the ambiant magnetic field (angle and direction : sunward or anti-sunward) . A statistical study of the inclination of these waves and of their parameters is presented and allows us to make assumptions about their roles. Single events are also presented in details
Published: 2022

6. Observations of the Time Domain Sampler receiver from the Radio and Plasma Wave instrument during the Solar Orbiter Earth flyby

Author: David Pisa, Jan Soucek, Ondrej Santolik, Miroslav Hanzelka, Milan Maksimovic, Antonio Vecchio, Yuri Khotyaintsev, Thomas Chust, Matthieu Kretzschmar, Lorenzo Matteini, and Timothy Horbury
Abstract: On November 27, 2021, Solar Orbiter completed its only flyby of Earth on its way to the following Sun’s encounter in March 2022. Although this fast flyby was performed primarily to decrease the spacecraft’s velocity and change orbit to get closer to the Sun, the Radio and Plasma Wave (RPW) instrument had the opportunity to perform high cadence measurements in the Earth’s magnetosphere. We review the main observation of the Time Domain Sampler (TDS) receiver, a part of the RPW instrument, made during this flyby at frequencies below 200 kHz. The TDS receiver operated in a high cadence mode providing us with the regular waveform snapshot with 62 ms length every ten seconds for two electric components. Besides the regular captures, we have got more than five hundred onboard classified snapshots and the statistical products with a sixteen-second cadence. Before entering the terrestrial magnetosphere around 02:30UT, the spacecraft wandered through the foreshock region, registering intense bursts of Langmuir waves. After the bowshock crossing, Solar Orbiter was for more than two hours in the morning sector of the magnetosphere, recording various plasma wave modes. The closest approach was reached at 04:30UT above North Africa at an altitude of 460 km. Then the spacecraft continued into the Earth’s tail and entered the magnetosheath around 13:00UT. After 15:00UT, the Solar Orbiter crossed the bowshock, and bursts of Langmuir waves were detected again pointing out to the deep downstream foreshock region. Further from the Earth, intense Auroral Kilometric Radiation (AKR) at frequencies above 100 kHz was also detected.
Published: 2022

7. Polarization of Langmuir waves observed by RPW-TDS instrument on Solar Orbiter during Type III radio bursts

Author: Jan Soucek, Sampath Bandara, David Pisa, Ondrej Santolik, Milan Maksimovic, Thomas Chust, Yuri Khotyaintsev, Antonio Vecchio, Matthieu Kretzschmar, Robert Wimmer-Schweingruber, Lars Berger, Javier Rodriquez-Pacheco, and Raul Gomez-Herrero
Abstract: We investigate the polarization of Langmuir waves observed by the Time Domain Sampler (TDS) module of the Radio and Plasma Waves instrument on Solar Orbiter during several extensive Type III burst events. During its two-year-long cruise phase, Solar orbiter often crossed the source region of the Type III radio emission and observed the Langmuir waves generated by solar energetic electrons. The waves are known to exhibit complex modulation and often non-trivial elliptical polarization which sometimes rapidly changes on the timescales of tens of milliseconds. We show that the observed waveforms are typically composed of multiple sub-packets with a relatively short coherence length. We investigate the correlation between the polarization of the waves, simultaneously observed energetic electrons beams and other plasma properties.
Published: 2022

8. ICARUS: in-situ studies of the solar corona beyond Parker Solar Probe and Solar Orbiter

Author: Vladimir Krasnoselskikh, Bruce T. Tsurutani, Thierry Dudok de Wit, Simon Walker, Michael Balikhin, Marianne Balat-Pichelin, Marco Velli, Stuart D. Bale, Milan Maksimovic, Oleksiy Agapitov, Wolfgang Baumjohann, Matthieu Berthomier, Roberto Bruno, Steven R. Cranmer, Bart de Pontieu, Domingos de Sousa Meneses, Jonathan Eastwood, Robertus Erdelyi, Robert Ergun, Viktor Fedun, Natalia Ganushkina, Antonella Greco, Louise Harra, Pierre Henri, Timothy Horbury, Hugh Hudson, Justin Kasper, Yuri Khotyaintsev, Matthieu Kretzschmar, Säm Krucker, Harald Kucharek, Yves Langevin, Benoît Lavraud, Jean-Pierre Lebreton, Susan Lepri, Michael Liemohn, Philippe Louarn, Eberhard Moebius, Forrest Mozer, Zdenek Nemecek, Olga Panasenco, Alessandro Retino, Jana Safrankova, Jack Scudder, Sergio Servidio, Luca Sorriso-Valvo, Jan Souček, Adam Szabo, Andris Vaivads, Grigory Vekstein, Zoltan Vörös, Teimuraz Zaqarashvili, Gaetano Zimbardo, Andrei Fedorov, 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), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-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), 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: Space and Planetary Science, [SDU]Sciences of the Universe [physics], Solar wind, Solar atmosphere, Astronomy and Astrophysics, Space mission, Heliophysics
Abstract: The primary scientific goal of ICARUS (Investigation of Coronal AcceleRation and heating of solar wind Up to the Sun), a mother-daughter satellite mission, proposed in response to the ESA “Voyage 2050” Call, will be to determine how the magnetic field and plasma dynamics in the outer solar atmosphere give rise to the corona, the solar wind, and the entire heliosphere. Reaching this goal will be a Rosetta Stone step, with results that are broadly applicable within the fields of space plasma physics and astrophysics. Within ESA’s Cosmic Vision roadmap, these science goals address Theme 2: “How does the Solar System work?” by investigating basic processes occurring “From the Sun to the edge of the Solar System”. ICARUS will not only advance our understanding of the plasma environment around our Sun, but also of the numerous magnetically active stars with hot plasma coronae. ICARUS I will perform the first direct in situ measurements of electromagnetic fields, particle acceleration, wave activity, energy distribution, and flows directly in the regions in which the solar wind emerges from the coronal plasma. ICARUS I will have a perihelion altitude of 1 solar radius and will cross the region where the major energy deposition occurs. The polar orbit of ICARUS I will enable crossing the regions where both the fast and slow winds are generated. It will probe the local characteristics of the plasma and provide unique information about the physical processes involved in the creation of the solar wind. ICARUS II will observe this region using remote-sensing instruments, providing simultaneous, contextual information about regions crossed by ICARUS I and the solar atmosphere below as observed by solar telescopes. It will thus provide bridges for understanding the magnetic links between the heliosphere and the solar atmosphere. Such information is crucial to our understanding of the plasma physics and electrodynamics of the solar atmosphere. ICARUS II will also play a very important relay role, enabling the radio-link with ICARUS I. It will receive, collect, and store information transmitted from ICARUS I during its closest approach to the Sun. It will also perform preliminary data processing before transmitting it to Earth. Performing such unique in situ observations in the area where presumably hazardous solar energetic particles are energized, ICARUS will provide fundamental advances in our capabilities to monitor and forecast the space radiation environment. Therefore, the results from the ICARUS mission will be extremely crucial for future space explorations, especially for long-term crewed space missions.
Published: 2022

9. Global Energetics of Solar Flares. V. Energy Closure in Flares and Coronal Mass Ejections

Author: Markus J Aschwanden, Amir Caspi, Christina M S Cohen, Gordon Holman, Ju Jing, Matthieu Kretzschmar, Eduard P Kontar, James M McTiernan, Richard A Mewaldt, Aidan O'Flannagain, Ian G Richardson, Daniel Ryan, Harry P Warren, and Yan Xu
Subjects: Solar Physics
Abstract: In this study we synthesize the results of four previous studies on the global energetics of solar flares and associated coronal mass ejections (CMEs), which include magnetic, thermal, nonthermal, and CME energies in 399 solar M and X-class flare events observed during the first 3.5 years of the Solar Dynamics Observatory (SDO) mission. Our findings are: (1) The sum of the mean nonthermal energy of flare-accelerated particles (E(sub nt)), the energy of direct heating (E(sub dir)), and the energy in coronal mass ejections (E(sub CME)), which are the primary energy dissipation processes in a flare, is found to have a ratio of (E(sub nt)+E(sub dir)+E(sub CME))/E(sub mag) = 0.87±0.18, compared with the dissipated magnetic free energy E(sub mag), which confirms energy closure within the measurement uncertainties and corroborates the magnetic origin of flares and CMEs; (2) The energy partition of the dissipated magnetic free energy is: 0.51±0.17 in nonthermal energy of ≥ 6 keV electrons, 0.17± 0.17 in nonthermal ≥ 1 MeV ions, 0.07 ± 0.14 in CMEs, and 0.07 ± 0.17 in direct heating; (3) The thermal energy is almost always less than the nonthermal energy, which is consistent with the thick-target model; (4) The bolometric luminosity in white-light flares is comparable with the thermal energy in soft X-rays (SXR); (5) Solar Energetic Particle (SEP) events carry a fraction ≈ 0.03 of the CME energy, which is consistent with CME-driven shock acceleration; and (6) The warm-target model predicts a lower limit of the low-energy cutoff at ec ≈ 6 keV, based on the mean differential emission measure (DEM) peak temperature of T(sub e) = 8.6 MK during flares. This work represents the first statistical study that establishes energy closure in solar flare/CME events.
Published: 2017
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10. Whistler instability driven by the sunward electron deficit in the solar wind: High-cadence Solar Orbiter observations

Author: Matthieu Berthomier, V. Fortunato, Thomas Chust, Stefano Livi, Dhiren Kataria, Christopher J. Owen, Yuri V. Khotyaintsev, C. Anekallu, Etienne Behar, Christopher W. Kelly, Daniel Verscharen, Lucas Colomban, Roberto Bruno, G. Mele, Matthieu Kretzschmar, Milan Maksimovic, Laura Berčič, Philippe Louarn, Georgios Nicolaou, G. Watson, Robert T. Wicks, and Gethyn R. Lewis
Subjects: 010504 meteorology & atmospheric sciences, Whistler, Wave propagation, F300, Astrophysics, Electron, F500, 01 natural sciences, Electromagnetic radiation, law.invention, Orbiter, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Computer Science::Information Retrieval, Astronomy and Astrophysics, Plasma, Computational physics, Solar wind, Heat flux, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Context. Solar wind electrons play an important role in the energy balance of the solar wind acceleration by carrying energy into interplanetary space in the form of electron heat flux. The heat flux is stored in the complex electron velocity distribution functions (VDFs) shaped by expansion, Coulomb collisions, and field-particle interactions. Aims. We investigate how the suprathermal electron deficit in the anti-strahl direction, which was recently discovered in the near-Sun solar wind, drives a kinetic instability and creates whistler waves with wave vectors that are quasi-parallel to the direction of the background magnetic field. Methods. We combined high-cadence measurements of electron pitch-angle distribution functions and electromagnetic waves provided by Solar Orbiter during its first orbit. Our case study is based on a burst-mode data interval from the Electrostatic Analyser System (SWA-EAS) at a distance of 112 RS (0.52 au) from the Sun, during which several whistler wave packets were detected by Solar Orbiter’s Radio and Plasma Waves (RPW) instrument. Results. The sunward deficit creates kinetic conditions under which the quasi-parallel whistler wave becomes unstable. We directly test our predictions for the existence of these waves through solar wind observations. We find whistler waves that are quasi-parallel and almost circularly polarised, propagating away from the Sun, coinciding with a pronounced sunward deficit in the electron VDF. The cyclotron-resonance condition is fulfilled for electrons moving in the direction opposite to the direction of wave propagation, with energies corresponding to those associated with the sunward deficit. Conclusions. We conclude that the sunward deficit acts as a source of quasi-parallel whistler waves in the solar wind. The quasilinear diffusion of the resonant electrons tends to fill the deficit, leading to a reduction in the total electron heat flux.
Published: 2021

11. Solar Orbiter/RPW antenna calibration in the radio domain and its application to type III burst observations

Author: M. Steller, Milan Maksimovic, M. Dekkali, E. Lorfèvre, Vratislav Krupar, Antonio Vecchio, Arnaud Zaslavsky, Stuart D. Bale, Yu. V. Khotyaintsev, Vladimir Krasnoselskikh, Štěpán Štverák, Matthieu Kretzschmar, P. L. Astier, Dirk Plettemeier, Xavier Bonnin, Pavel M. Trávníček, J. Soucek, Andris Vaivads, E. Guilhem, T. Chust, Baptiste Cecconi, 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), ALTRAN (FRANCE), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, 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), and Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, Domain (software engineering), Fusion, plasma och rymdfysik, Orbiter, Astronomi, astrofysik och kosmologi, Physics - Space Physics, law, Antenna calibration, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Aerospace engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), detectors, 0105 earth and related environmental sciences, instrumentation, Physics, Sun: radio radiation, business.industry, instrumentation: detectors, Computer Science::Information Retrieval, Sun, Astronomy and Astrophysics, Fusion, Plasma and Space Physics, Space Physics (physics.space-ph), Astrophysics - Solar and Stellar Astrophysics, solar wind, Space and Planetary Science, radio radiation, Astrophysics - Instrumentation and Methods for Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Context.In order to allow for a comparison with the measurements from other antenna systems, the voltage power spectral density measured by the Radio and Plasma waves receiver (RPW) on board Solar Orbiter needs to be converted into physical quantities that depend on the intrinsic properties of the radiation itself (e.g., the brightness of the source).Aims.The main goal of this study is to perform a calibration of the RPW dipole antenna system that allows for the conversion of the voltage power spectral density measured at the receiver’s input into the incoming flux density.Methods.We used space observations from the Thermal Noise Receiver (TNR) and the High Frequency Receiver (HFR) to perform the calibration of the RPW dipole antenna system. Observations of type III bursts by the Wind spacecraft are used to obtain a reference radio flux density for cross-calibrating the RPW dipole antennas. The analysis of a large sample of HFR observations (over about ten months), carried out jointly with an analysis of TNR-HFR data and prior to the antennas’ deployment, allowed us to estimate the reference system noise of the TNR-HFR receivers.Results.We obtained the effective length,leff, of the RPW dipoles and the reference system noise of TNR-HFR in space, where the antennas and pre-amplifiers are embedded in the solar wind plasma. The obtainedleffvalues are in agreement with the simulation and measurements performed on the ground. By investigating the radio flux intensities of 35 type III bursts simultaneously observed by Wind and Solar Orbiter, we found that while the scaling of the decay time as a function of the frequency is the same for the Waves and RPW instruments, their median values are higher for the former. This provides the first observational evidence that Type III radio waves still undergo density scattering, even when they propagate from the source, in a medium with a plasma frequency that is well below their own emission frequency.
Published: 2021

12. The Solar Orbiter Radio and Plasma Waves (RPW) instrument (Corrigendum)

Author: Andris Vaivads, V. Krupař, M. Chariet, Lars Bylander, L. R. Malac-Allain, J. Parisot, Mats André, W. Recart, W. Puccio, C. Agrapart, D. Bérard, V. Leray, Robert F. Wimmer-Schweingruber, K. Boughedada, Baptiste Cecconi, E. Lorfèvre, M. Steller, B. Katra, F. Chapron, Helmut O. Rucker, Stuart D. Bale, Matthieu Kretzschmar, J.-C. Pellion, Ivana Kolmasova, J. Sanisidro, N. Quéruel, Filippo Pantellini, V. Bouzid, Laurent Lamy, Milan Maksimovic, L. Guéguen, C. Fiachetti, S. Chaintreuil, Mykhaylo Panchenko, Karine Issautier, M. Dekkali, O. Krupařová, Keith Goetz, Tomas Karlsson, I. Fratter, H. Ottacher, Philippe Louarn, P. Fergeau, O. Le Contel, Christopher J. Owen, Jan Soucek, A. Retino, Mihailo M. Martinović, Y. de Conchy, Olga Alexandrova, E. Bellouard, G. T. Delory, David Pisa, S. Thijs, E. Guilhem, Anders Eriksson, L. Åhlén, Antonio Vecchio, Timothy S. Horbury, Ondrej Santolik, Eduard P. Kontar, T. Vincent, V. Cripps, Daniel Dias, I. Zouganelis, A. Jeandet, T. Dudok de Wit, Sonny Lion, L. Uhlíř, Quynh Nhu Nguyen, M. Timofeeva, Dirk Plettemeier, J. Baše, Christopher Cully, Petr Hellinger, Lorenzo Matteini, Fouad Sahraoui, C. Collin, Paul Turin, Javier Rodriguez-Pacheco, Säm Krucker, P. Plasson, J.-Y. Brochot, Vladimir Krasnoselskikh, P. Leroy, Petr Travnicek, R. Lán, Yu. V. Khotyaintsev, S.-E. Jansson, Štěpán Štverák, G. Barbary, Pierre Astier, G. Jannet, R. Piberne, E. P. G. Johansson, F. Gonzalez, P. Danto, Arnaud Zaslavsky, J. Břínek, Thomas Chust, Xavier Bonnin, C. Laffaye, G. Cassam-Chenai, S. Julien, B. Pontet, Matthieu Berthomier, 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), 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), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Commission for Astronomy of the Austrian Academy of Sciences, Austrian Academy of Sciences (OeAW), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Space Research Institute of Austrian Academy of Sciences (IWF), Royal Institute of Technology [Stockholm] (KTH ), 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), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Nexeya Conseil & Formation, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen], Centre National d'Études Spatiales [Toulouse] (CNES), Centre d’Ecologie Fonctionnelle et Evolutive (CEFE), Université Paul-Valéry - Montpellier 3 (UPVM)-Centre international d'études supérieures en sciences agronomiques (Montpellier SupAgro)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Institut national d’études supérieures agronomiques de Montpellier (Montpellier SupAgro), Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), ALTRAN (FRANCE), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), Univerzita Karlova v Praze, Universities Space Research Association (USRA), NASA Goddard Space Flight Center (GSFC), Department of Physics and Astronomy [Calgary], University of Calgary, School of Physics and Astronomy [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Department of Physics [Imperial College London], Imperial College London, University of Glasgow, Fachhochschule Nordwestschweiz [Windisch] (FHNW), 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), Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, University of Belgrade [Belgrade], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Universidad de Alcalá - University of Alcalá (UAH), Institute of Experimental and Applied Physics [Kiel] (IEAP), Christian-Albrechts-Universität zu Kiel (CAU), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Radboud University [Nijmegen], Université Paul-Valéry - Montpellier 3 (UPVM)-École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut Agro - Montpellier SupAgro, Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro)-Institut national d'enseignement supérieur pour l'agriculture, l'alimentation et l'environnement (Institut Agro), Université de Rennes (UR), 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 Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: Physics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Astrophysics, Plasma, 01 natural sciences, law.invention, instrumentation: miscellaneous, Solar wind, Orbiter, solar wind, Space and Planetary Science, law, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, addenda, ComputingMilieux_MISCELLANEOUS, errata
Abstract: Contains fulltext : 239392.pdf (Publisher’s version ) (Open Access)
Published: 2021

13. Whistler wave occurrence and the interaction with strahl electrons during the first encounter of Parker Solar Probe

Author: Jasper Halekas, Michel Moncuquet, Justin C. Kasper, Vladimir Krasnoselskikh, Michael L. Stevens, Oleksiy Agapitov, A. Larosa, Stuart D. Bale, Kelly E. Korreck, L. Bercic, T. Dudok de Wit, Marc Pulupa, Matthieu Kretzschmar, Anthony W. Case, Clara Froment, Phyllis Whittlesey, Davin Larson, David M. Malaspina, V. K. Jagarlamudi, 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), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], University of Colorado [Boulder], University of California, Imperial College London, Queen Mary University of London (QMUL), Smithsonian Astrophysical Observatory, Smithsonian Institution, University of Michigan [Ann Arbor], University of Michigan System, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (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 Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: 010504 meteorology & atmospheric sciences, Whistler, FOS: Physical sciences, Electron, magnetic fields, 01 natural sciences, Electromagnetic radiation, Physics - Space Physics, 0103 physical sciences, waves, Sun: heliosphere, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], scattering, Astronomy and Astrophysics, plasmas, Space Physics (physics.space-ph), [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Computational physics, Magnetic field, Strahl, Solar wind, Amplitude, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Electron temperature
Abstract: We studied the properties and occurrence of narrow band whistler waves and their interaction with strahl electrons observed between 0.17 and 0.26 au during the first encounter of Parker Solar Probe. We observe that occurrence of whistler waves is low, nearly 1.5% and less than 0.5% in the analyzed peak and average BPF data respectively. Whistlers occur highly intermittently and 80% of the whistlers appear continuously for less than 3 s. Occurrence rate of whistler waves was found to be anti-correlated with the solar wind bulk velocity. The study of the duration of the whistler intervals revealed an anti-correlation between the duration and the solar wind velocity, as well as between the duration and the normalized amplitude of magnetic field variations. The pitch-angle widths (PAWs) of the field-aligned electron population referred to as the strahl are broader by at least 12 degrees during the presence of large amplitude narrow band whistler waves. This observation points towards a EM wave electron interaction, resulting in pitch-angle scattering. PAW of strahl electrons corresponding to the short duration whistlers are higher compared to the long duration whistlers. Parallel cuts through the strahl electron velocity distribution function (VDF) observed during the whistler intervals appear to depart from the Maxwellian shape typically found in the near-Sun strahl VDFs (Bercic et al. 2020). The relative decrease of parallel electron temperature and the increase of PAW for the electrons in strahl energy range suggests that the interaction with whistler waves results in a transfer of electron momentum from the parallel to the perpendicular direction., Comment: Accepted for publication in Astronomy & Astrophysics PSP special issue on January 12, 2021
Published: 2021

14. Solar Orbiter/Radio and Plasma Wave observations during the first Venus flyby

Author: Yuri V. Khotyaintsev, Antonio Vecchio, Niklas J. T. Edberg, Timothy S. Horbury, Matthieu Kretzschmar, Lina Hadid, Thomas Chust, Štěpán Štverák, V. Krasnoselskikh, Jan Soucek, M. Steller, Dirk Plettemeier, Stuart D. Bale, Andris Vaivads, E. Lorfèvre, Milan Maksimovic, Pavel M. Trávníček, Swedish Institute of Space Physics [Uppsala] (IRF), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of California, 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), Centre National d'Études Spatiales [Toulouse] (CNES), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Czech Academy of Sciences [Prague] (CAS), Austrian Academy of Sciences (OeAW), Royal Institute of Technology [Stockholm] (KTH ), Radboud university [Nijmegen], and Imperial College London
Subjects: Physics, Orbiter, biology, law, Waves in plasmas, Physics::Space Physics, Astronomy, Venus, Astrophysics::Earth and Planetary Astrophysics, biology.organism_classification, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 7. Clean energy, law.invention
Abstract: We present measurements from the Radio and Plasma Wave (RPW) instrument suite onboard the Solar Orbiter mission during the first Venus encounter. RPW consists of several units and is capable of measuring both the electric and magnetic field fluctuations with three electric antennas and a search-coil magnetometer: The Low Frequency Receiver (LFR) cover the range from DC up to 10kHz when measuring the electric and magnetic waveform and spectra; the Thermal Noise and High Frequency Receiver (TNR-HFR) determines the electric power spectra and magnetic power spectra from 4kHz-20MHz, and 4kHz to 500kHz, respectively, to determine properties of the electron population; the Time Domain Sampler (TDS) measures and digitizes onboard the electric and magnetic field waveforms from 100 Hz to 250 kHz. The BIAS subunit measures DC and LF electric fields as well as the spacecraft potential, which gives a high cadence measure of the local plasma density when calibrated to the low-cadence tracking of the plasma peak from the TNR. Solar Orbiter approached Venus from the induced magnetotail and had its closest approach at an altitude of 7500 km over the north pole of Venus on 27 Dec 2020. The RPW instruments observed a tail region that extended several 10’s of Venus radii downstream of the planet. The induced magnetosphere was characterized to be a highly dynamic environment as Solar Orbiter traversed the downstream tail and magnetosheath before it crossed the Bow Shock outbound at ~12:40 UT. Polarized whistler waves, high frequency electrostatic waves, narrow-banded emissions, possible electron double layers were observed. The fine structure of the bow shock could also be investigated in detail. Solar Orbiter could hence enhance the knowledge of the structure of the solar wind-Venus interaction.
Published: 2021

15. Impact induced electric field signals observed by the Solar Orbiter/RPW

Author: Stuart D. Bale, Thomas Chust, Dirk Plettemeier, Milan Maksimovic, Matthieu Kretzschmar, M. Steller, Niklas J. T. Edberg, Antonio Vecchio, Michiko Morooka, Anders Eriksson, Štěpán Štverák, Jan Soucek, Erik M. J. Johansson, Andris Vaivads, Yuri V. Khotyaintsev, V. Krasnoselskikh, Pavel M. Trávníček, E. Lorfèvre, Swedish Institute of Space Physics [Uppsala] (IRF), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of California, Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-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), 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), Université d'Orléans (UO), Centre National d'Études Spatiales [Toulouse] (CNES), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Czech Academy of Sciences [Prague] (CAS), Austrian Academy of Sciences (OeAW), Royal Institute of Technology [Stockholm] (KTH ), and Radboud university [Nijmegen]
Subjects: Physics, Orbiter, Optics, law, business.industry, [SDU]Sciences of the Universe [physics], Electric field, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, law.invention
Abstract: A large-amplitude impact-induced like electric field signal is often observed by the Radio and Plasma Wave (RPW) Instrument onboard Solar Orbiter. The signal has a sharp increase followed by an exponential decay, typically observed when spacecraft experiences a dust impact. The amplitude can reach several V/m. The impact dust size can be estimated from the electric field amplitude and is similar to the characteristic dust size near the sun expected from the zodiacal-light observations. On the other hand, the signal's decay time is the order of second, unusually long compared to the dust impact signals previously reported by the other spacecraft. We will show the characteristics of these signals and discuss the origin.
Published: 2021

16. Search for oblique Whistler waves using solar orbiter data

Author: Laura Berčič, Milan Maksimovic, Lucas Colomban, Matthieu Kretzschmar, V. Krasnoselskikh, and Christopher J. Owen
Subjects: Orbiter, Whistler, law, Oblique case, Geophysics, Geology, law.invention
Abstract: Whistler waves are thought to play an important role on the evolution of the electron distribution function as a function of distance. In particular, oblique whistler waves may diffuse the Strahl electrons into the halo population. Using AC magnetic field from the RPW/SCM (search coil magnetometer) of Solar Orbiter, we search for the presence of oblique Whistler waves in the frequency range between 3 Hz and 128 Hz . We perform a minimum variance analysis of the SCM data in combination with the MAG (magnetometer) data to determine the inclination of the waves with respect to the ambiant magnetic field. As the emphasis is placed on the search for oblique whistler, we also analyze the RPW electric field data and the evolution of the electron distribution function during these Whistler events.
Published: 2021

17. Thin current sheets and the associated wave activity observed by Solar Orbiter

Author: Daniel B. Graham, Anders Eriksson, Milan Maksimovic, Thomas Chust, Yuri V. Khotyaintsev, Erik M. J. Johansson, Niklas J. T. Edberg, Konrad Steinvall, Matthieu Kretzschmar, Andris Vaivads, Swedish Institute of Space Physics [Uppsala] (IRF), Royal Institute of Technology [Stockholm] (KTH ), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-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), 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, and 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)
Subjects: [PHYS]Physics [physics], Orbiter, Optics, Materials science, 13. Climate action, business.industry, law, Physics::Space Physics, Current (fluid), business, law.invention
Abstract: Thin current sheets are routinely observed in the solar wind. Here we report observations of thin current sheets and the associated plasma waves using the Solar Orbiter spacecraft. The Radio and Plasma Waves (RPW) instrument provides high-resolution measurements of the electric field, number density perturbations, and magnetic field fluctuations, which we use to identify and characterise the observed waves, while the magnetic field provided by the MAG instrument is used to characterise the current sheets. We discuss the role of current sheets in the generation of the observed waves and the effects of the waves on the current sheets.
Published: 2021

18. Decomposition of the switchback boundary on MHD wave modes

Author: F. S. Mozer, Thierry Dudok de Wit, Peter Harvey, Davin Larson, Claire Reveillet, A. Larosa, Justin C. Kasper, Vamsee Krishna Jagarlamudi, Clara Froment, Matthieu Kretzschmar, Kelly E. Korreck, Marc Pulupa, Keith Goetz, Oleksiy Agapitov, Vladimir Krasnoselskikh, Michael L. Stevens, Marco Velli, Robert J. MacDowall, David M. Malaspina, and Stuart D. Bale
Subjects: Physics, Decomposition (computer science), Boundary (topology), Mechanics, Magnetohydrodynamics
Abstract: Switchback boundaries separate two plasmas moving with different velocities, that may have different temperatures and densities and typically manifest sharp magnetic field deflections through the boundary. They may be analyzed similarly to MHD discontinuities. The first step of their characterization consists of analysis in terms of MHD discontinuities. Such an analysis was performed by Larosa et al., (2021) who has found that 32% of them may be attributed to rotational discontinuities, 17% to tangential, about 42% to the group of discontinuities that are difficult to unambiguously define whether they are tangential or rotational, and 9% that do not belong to any of these two groups. We describe and apply hereafter for two events another approach for the characterization of the boundaries based on classification of the general type discontinuity in MHD approximation. It is based on the problem of the decay of the general type of discontinuity. It is well known [Kulikovsky and Lyubimov, 1962, Gogosov, 1959} that general type MHD discontinuity decays on 7 separate discontinuities belonging to different types of MHD waves, namely, entropic wave, two slow mode waves, two Alfvenic waves, and two fast mode waves. Entropic wave is standing in the reference frame of the discontinuity; other wave modes are supposed to run in the opposite directions from the initial discontinuity with their characteristic velocities. Making use of plasma parameters from two sides of the boundary one can evaluate the fraction of each wave mode present in the discontinuity. We apply this method to two boundary crossings. This repartition of the discontinuity allows characterizing the deviation from Alfvenicity quantitatively.ReferencesLarosa, A., et al., A&A, 2021, (accepted)Kulikovsky, Lyubimov, Magnetohydrodynamics, (1962)Gogosov, V.V., Decay of the MHD discontinuity, (1959)
Published: 2021

19. Direct evidence for magnetic reconnection at the boundaries of magnetic switchbacks with Parker Solar Probe

Author: Vladimir Krasnoselskikh, Marco Velli, Robert J. MacDowall, Phyllis Whittlesey, Anthony W. Case, Davin Larson, T. Dudok de Wit, Keith Goetz, Marc Pulupa, Benoit Lavraud, Justin C. Kasper, David M. Malaspina, Vamsee Krishna Jagarlamudi, Kelly E. Korreck, N. Fargette, Clara Froment, Oleksiy Agapitov, A. Larosa, Stuart D. Bale, F. S. Mozer, C. Revillet, Michael L. Stevens, Matthieu Kretzschmar, 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), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Colorado [Boulder], Smithsonian Astrophysical Observatory, Smithsonian Institution, School of Physics and Astronomy [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Department of Climate and Space Sciences and Engineering (CLaSP), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, GSFC Solar System Exploration Division, NASA Goddard Space Flight Center (GSFC), IACR Brooms Barn, Partenaires INRAE, University of California [Berkeley], University of California-University of California, 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: Field (physics), FOS: Physical sciences, Context (language use), Solar radius, Astrophysics, magnetic fields, 01 natural sciences, Current sheet, Physics - Space Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sun: heliosphere, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, Magnetic reconnection, Space Physics (physics.space-ph), Magnetic field, Solar wind, Astrophysics - Solar and Stellar Astrophysics, solar wind, Space and Planetary Science, magnetic reconnection, Physics::Space Physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere
Abstract: Parker Solar Probe's first encounters with the Sun revealed the presence of ubiquitous localised magnetic deflections in the inner heliosphere; these structures, often called switchbacks, are particularly striking in solar wind streams originating from coronal holes. We report the direct evidence for magnetic reconnection occuring at the boundaries of three switchbacks crossed by Parker Solar Probe (PSP) at a distance of 45 to 48 solar radii of the Sun during its first encounter. We analyse the magnetic field and plasma parameters from the FIELDS and SWEAP instruments. The three structures analysed all show typical signatures of magnetic reconnection. The ion velocity and magnetic field are first correlated and then anti-correlated at the inbound and outbound edges of the bifurcated current sheets with a central ion flow jet. Most of the reconnection events have a strong guide field and moderate magnetic shear but one current sheet shows indications of quasi anti-parallel reconnection in conjunction with a magnetic field magnitude decrease by $90\%$. Given the wealth of intense current sheets observed by PSP, reconnection at switchbacks boundaries appears to be rare. However, as the switchback boundaries accomodate currents one can conjecture that the geometry of these boundaries offers favourable conditions for magnetic reconnection to occur. Such a mechanism would thus contribute in reconfiguring the magnetic field of the switchbacks, affecting the dynamics of the solar wind and eventually contributing to the blending of the structures with the regular wind as they propagate away from the Sun., Comment: 11 pages, 7 figures, 2 tables, accepted for publication in A&A, PSP special issue (v2: typos correction)
Published: 2021

20. Measurement of magnetic field fluctuations in the Parker Solar Probe and Solar Orbiter missions

Author: E. Lorfèvre, Stuart D. Bale, G. Chalumeau, G. Jannet, P. Fergeau, J.-Y. Brochot, Milan Maksimovic, M. Bergerard-Timofeeva, T. Dudok de Wit, C. Revillet, E. Guilhem, P. Martin, Matthieu Kretzschmar, C. Brysbaert, Peter Harvey, Trevor A. Bowen, V. Krasnoselskikh, C. Agrapart, Keith Goetz, V. Leray, 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), 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)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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, and 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)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Magnetometer, Plasma, 01 natural sciences, Electromagnetic radiation, Computational physics, law.invention, Magnetic field, Orbiter, Search coil, Solar wind, Geophysics, Space and Planetary Science, law, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, 0105 earth and related environmental sciences
Abstract: International audience; The search‐coil magnetometer (SCM) measures the magnetic signature of solar wind fluctuations with three components in the 3 Hz – 50 kHz range and one single component in the 1 kHz – 1 MHz range. This instrument is important for providing in situ observations of transients caused by interplanetary shocks and reconnection, for the identification of electromagnetic wave modes in plasmas and the determination of their characteristics (planarity, polarization, ellipticity and k‐vector) and for studying the turbulent cascade in the kinetic range. Two similar triaxial search‐coils have been built for the Parker Solar Probe and Solar Orbiter missions. Here we describe the science objectives of both missions which led to the SCM design and present the characteristics of the two instruments.
Published: 2021

21. The Solar Orbiter Radio and Plasma Waves (RPW) instrument

Author: L. R. Malac-Allain, T. Dudok de Wit, E. Lorfèvre, C. Collin, J. Sanisidro, Mihailo M. Martinović, X. Bonnin, E. Guilhem, Milan Maksimovic, P. Leroy, A. Vecchio, Eduard P. Kontar, L. Uhlíř, N. Quéruel, H. Ottacher, K. Boughedada, Christopher Cully, G. Barbary, Pierre Astier, Anders Eriksson, L. Åhlén, O. Krupařová, B. Pontet, T. Chust, G. Jannet, J. Parisot, Mats André, Paul Turin, P. Plasson, F. Chapron, M. Steller, W. Recart, W. Puccio, Vladimir Krasnoselskikh, Robert F. Wimmer-Schweingruber, V. Bouzid, Laurent Lamy, V. Cripps, R. Lán, Keith Goetz, B. Katra, S. Chaintreuil, Gregory T. Delory, I. Fratter, Dirk Plettemeier, C. Fiachetti, V. Krupař, M. Chariet, Sonny Lion, M. Dekkali, Lars Bylander, F. Gonzalez, Jan Soucek, Christopher J. Owen, Mykhaylo Panchenko, P. Danto, David Pisa, T. Vincent, Y. de Conchy, Säm Krucker, G. Cassam-Chenai, S. Julien, Baptiste Cecconi, Olga Alexandrova, A. Retino, V. Leray, Karine Issautier, S. Thijs, E. P. G. Johansson, Filippo Pantellini, D. Bérard, J. Baše, L. Guéguen, R. Piberne, P. Fergeau, Matthieu Berthomier, Tomas Karlsson, Arnaud Zaslavsky, Quynh Nhu Nguyen, J.-Y. Brochot, E. Bellouard, Yu. V. Khotyaintsev, Lorenzo Matteini, Štěpán Štverák, Javier Rodriguez-Pacheco, Fouad Sahraoui, S.-E. Jansson, O. Le Contel, Timothy S. Horbury, J.-C. Pellion, Pavel M. Trávníček, A. Jeandet, C. Agrapart, Petr Hellinger, Ondrej Santolik, I. Zouganelis, C. Laffaye, M. Timofeeva, D. Dias, Philippe Louarn, Helmut O. Rucker, Stuart D. Bale, Ivana Kolmasova, J. Břínek, Matthieu Kretzschmar, Andris Vaivads, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), 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), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Institute of Computing [Campinas] (IC), Universidade Estadual de Campinas = University of Campinas (UNICAMP), Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Centre d'Investigation Clinique [CHU Clermont-Ferrand] (CIC 1405), Institut National de la Santé et de la Recherche Médicale (INSERM)-Direction de la recherche clinique et de l’innovation [CHU Clermont-Ferrand] (DRCI), CHU Clermont-Ferrand-CHU Clermont-Ferrand, Department of Physics [Imperial College London], Imperial College London, Laboratoire Structures, Propriétés et Modélisation des solides (SPMS), Institut de Chimie du CNRS (INC)-CentraleSupélec-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Hasselt University (UHasselt), Centre National d'Études Spatiales [Toulouse] (CNES), Centre National d’Etudes Spatiales, Centre National d’Études Spatiales [Paris] (CNES), 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), DIREN RHONE ALPES LYON FRA, Partenaires IRSTEA, Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), International Agency for Research on Cancer (IARC), Institute of Genetics and Molecular Medicine, University of Edinburgh, Centre Hospitalier Régional Universitaire [Montpellier] (CHRU Montpellier), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), NASA Goddard Space Flight Center (GSFC), Universities Space Research Association (USRA), Jiangsu University of Science and Technology (JUST), Universidade Estadual Paulista Júlio de Mesquita Filho = São Paulo State University (UNESP), Alfven Laboratory, Royal Institute of Technology [Stockholm] (KTH ), Department of Plant Physiology, Umeå University, Umea Plant Science Centre, Umeå University-Umeå University, Swedish University of Agricultural Sciences (SLU), Department of Space and Plasma Physics [Stockholm], KTH School of Electrical Engineering, Royal Institute of Technology [Stockholm] (KTH )-Royal Institute of Technology [Stockholm] (KTH ), Swedish Institute of Space Physics [Kiruna] (IRF), 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), Agence Spatiale Européenne = European Space Agency (ESA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institute of Computing [Campinas] (UNICAMP), Universidade Estadual de Campinas (UNICAMP), Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley], University of California-University of California, 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 (European Space Agency) (ESA)
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, Plasma oscillation, 01 natural sciences, law.invention, Orbiter, Astronomi, astrofysik och kosmologi, law, 0103 physical sciences, Astronomy, Astrophysics and Cosmology, Aerospace engineering, 010303 astronomy & astrophysics, miscellaneous [instrumentation], 0105 earth and related environmental sciences, Physics, business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Plasma, Solar radio, instrumentation: miscellaneous, Solar wind, solar wind, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Interplanetary spaceflight, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter mission is described in this paper. This instrument is designed to measure in-situ magnetic and electric fields and waves from the continuous to a few hundreds of kHz. RPW will also observe solar radio emissions up to 16 MHz. The RPW instrument is of primary importance to the Solar Orbiter mission and science requirements since it is essential to answer three of the four mission overarching science objectives. In addition RPW will exchange on-board data with the other in-situ instruments in order to process algorithms for interplanetary shocks and type III langmuir waves detections. Correction in: Astronomy & Astrophysics, Volume 654, Article Number C2, DOI 10.1051/0004-6361/201936214e
Published: 2020

22. The Solar Orbiter Science Activity Plan: Translating solar and heliospheric physics questions into action

Author: Jack Jenkins, A. Vecchio, Georgios Nicolaou, Robert T. Wicks, Sarah A. Matthews, Matthieu Berthomier, T. Chust, Johann Hirzberger, L. Dolla, R. Carr, Spiros Patsourakos, O. Alexandrova, R. De Marco, V. Da Deppo, Angelos Vourlidas, Vincent Génot, Martin M. Roth, Alessandro Bemporad, Eduard P. Kontar, Susan T. Lepri, Lucie M. Green, Pedro Osuna, Jon A. Linker, Sergio Toledo-Redondo, D. Orozco Suárez, Denise Perrone, I. Carrasco-Blazquez, Manolis K. Georgoulis, Achim Gandorfer, Hardi Peter, Daniele Spadaro, Dirk Plettemeier, N. J. Fox, Luciano Rodriguez, Olga Malandraki, Andrei Zhukov, Teresa Nieves-Chinchilla, A. Giunta, Natasha L. S. Jeffrey, L. Etesi, Karine Bocchialini, Davina Innes, Kévin Dalmasse, Jim M. Raines, Jesper Schou, J. C. del Toro Iniesta, Jonathan Eastwood, Lucia Abbo, P. Rochus, T. Dudok de Wit, T. Appourchaux, Stuart D. Bale, C. Watson, Milan Maksimovic, F. Espinosa Lara, Sami K. Solanki, Paulett C. Liewer, Matthieu Kretzschmar, Vincenzo Andretta, L. R. Bellot Rubio, C. Plainaki, C. Terasa, V. Martinez-Pillet, C. Gontikakis, Säm Krucker, S. Parenti, David Long, I. Zouganelis, Silvano Fineschi, Gary Graham, Sophie Musset, Daniel Müller, L. Sanchez, Robert F. Wimmer-Schweingruber, Lakshmi Pradeep Chitta, Xavier Bonnin, Hamish A. S. Reid, Stefano Livi, Thomas Wiegelmann, Andreas Lagg, N. Vilmer, David Berghmans, D. Fontaine, Arnaud Masson, Francesco Valentini, Fernando Carcaboso, Laurence Rezeau, Luca Sorriso-Valvo, I. Cernuda Cangas, David R. Williams, Shane A. Maloney, M. Haberreiter, Miho Janvier, Andrei Fedorov, Luca Teriaca, Timothy S. Horbury, Philippe Louarn, Benoit Lavraud, Christopher J. Owen, Donald M. Hassler, Georgia Tsiropoula, Etienne Pariat, L. van Driel-Gesztelyi, Athanasios Papaioannou, Nicole Meyer-Vernet, Daniel Verscharen, D. N. Baker, Federico Landini, Cis Verbeeck, S. Gissot, Louise K. Harra, L. Rodriguez-Garcia, Andrea Verdini, Baptiste Cecconi, Ioannis Kontogiannis, C. N. Arge, Andrew Walsh, Richard Morton, Marco Romoli, Daniele Telloni, Lorenzo Matteini, Eric Buchlin, Fouad Sahraoui, Roberto Bruno, Christopher H. K. Chen, Radoslav Bučík, Nicolas Labrosse, J. Lefort, K. Moraitis, N. Janitzek, Gethyn R. Lewis, M. Steller, Kostas Tziotziou, Holly Gilbert, Angels Aran, F. Felix-Redondo, Mathew J. Owens, A. S. Brun, Alexander Nindos, Alexander W. James, K. Issautier, Laurent Gizon, N. E. Raouafi, B. Fleck, Javier Rodriguez-Pacheco, Alexis P. Rouillard, Raul Gomez-Herrero, George C. Ho, R. A. Howard, G. J. Hurford, Raffaella D'Amicis, F. Auchère, Helen O'Brien, Andrzej Fludra, J. Büchner, A. Tsounis, Roberto Susino, C. Krafft, Yu. V. Khotyaintsev, Udo Schühle, Štěpán Štverák, Mihailo M. Martinović, Maurizio Pancrazzi, Guillaume Aulanier, S. P. Plunkett, Marco Stangalini, Rui F. Pinto, A. De Groof, David Stansby, Jan Soucek, S. Dolei, Andris Vaivads, Marina Battaglia, Antoine Strugarek, Anastasios Anastasiadis, K.-L. Klein, Peter R. Young, Clementina Sasso, Marco Velli, V. Krasnoselskikh, A. Retino, T. Grundy, I. Leon, O. C. St. Cyr, Ester Antonucci, European Space Agency (European Space Agency) (ESA), Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Saclay-Sorbonne Université-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-École polytechnique (X)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU), Centre National D'Etudes Spatiales (France), Agenzia Spaziale Italiana, Czech Grant Agency, National Aeronautics and Space Administration (US), Ministerio de Ciencia e Innovación (España), European Commission, Science and Technology Facilities Council (UK), and Science and Technology Facilities Council (STFC)
Subjects: Solar System, instruments [space vehicles], 010504 meteorology & atmospheric sciences, Astronomy, observational [methods], Astrophysics, 01 natural sciences, 7. Clean energy, law.invention, Methods: observational, law, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], general [Sun], Astrophysics::Solar and Stellar Astrophysics, Space vehicles: instruments, space vehicles: instruments, methods: observational, Sun: general, Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, MISSION, Physics, COORDINATION, INSTRUMENT, Astrophysics::Instrumentation and Methods for Astrophysics, Solar wind, Astrophysics - Solar and Stellar Astrophysics, Physics::Space Physics, Physical Sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, PAYLOAD, Sun: general, astro-ph.SR, TELESCOPE, F300, FOS: Physical sciences, F500, Astronomy & Astrophysics, Computer Science::Digital Libraries, REGION, Orbiter, 0201 Astronomical and Space Sciences, 0103 physical sciences, Aerospace engineering, Solar dynamo, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Science & Technology, Spacecraft, business.industry, Ecliptic, Astronomy and Astrophysics, WIND, Physics::History of Physics, 13. Climate action, Space and Planetary Science, Orbit (dynamics), business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere, astro-ph.IM
Abstract: All authors: Zouganelis, I.; De Groof, A.; Walsh, A. P.; Williams, D. R.; Müller, D.; St Cyr, O. C.; Auchère, F.; Berghmans, D.; Fludra, A.; Horbury, T. S.; Howard, R. A.; Krucker, S.; Maksimovic, M.; Owen, C. J.; Rodríguez-Pacheco, J.; Romoli, M.; Solanki, S. K.; Watson, C.; Sanchez, L.; Lefort, J.; Osuna, P.; Gilbert, H. R.; Nieves-Chinchilla, T.; Abbo, L.; Alexandrova, O.; Anastasiadis, A.; Andretta, V.; Antonucci, E.; Appourchaux, T.; Aran, A.; Arge, C. N.; Aulanier, G.; Baker, D.; Bale, S. D.; Battaglia, M.; Bellot Rubio, L.; Bemporad, A.; Berthomier, M.; Bocchialini, K.; Bonnin, X.; Brun, A. S.; Bruno, R.; Buchlin, E.; Büchner, J.; Bucik, R.; Carcaboso, F.; Carr, R.; Carrasco-Blázquez, I.; Cecconi, B.; Cernuda Cangas, I.; Chen, C. H. K.; Chitta, L. P.; Chust, T.; Dalmasse, K.; D'Amicis, R.; Da Deppo, V.; De Marco, R.; Dolei, S.; Dolla, L.; Dudok de Wit, T.; van Driel-Gesztelyi, L.; Eastwood, J. P.; Espinosa Lara, F.; Etesi, L.; Fedorov, A.; Félix-Redondo, F.; Fineschi, S.; Fleck, B.; Fontaine, D.; Fox, N. J.; Gandorfer, A.; Génot, V.; Georgoulis, M. K.; Gissot, S.; Giunta, A.; Gizon, L.; Gómez-Herrero, R.; Gontikakis, C.; Graham, G.; Green, L.; Grundy, T.; Haberreiter, M.; Harra, L. K.; Hassler, D. M.; Hirzberger, J.; Ho, G. C.; Hurford, G.; Innes, D.; Issautier, K.; James, A. W.; Janitzek, N.; Janvier, M.; Jeffrey, N.; Jenkins, J.; Khotyaintsev, Y.; Klein, K. -L.; Kontar, E. P.; Kontogiannis, I.; Krafft, C.; Krasnoselskikh, V.; Kretzschmar, M.; Labrosse, N.; Lagg, A.; Landini, F.; Lavraud, B.; Leon, I.; Lepri, S. T.; Lewis, G. R.; Liewer, P.; Linker, J.; Livi, S.; Long, D. M.; Louarn, P.; Malandraki, O.; Maloney, S.; Martinez-Pillet, V.; Martinovic, M.; Masson, A.; Matthews, S.; Matteini, L.; Meyer-Vernet, N.; Moraitis, K.; Morton, R. J.; Musset, S.; Nicolaou, G.; Nindos, A.; O'Brien, H.; Orozco Suarez, D.; Owens, M.; Pancrazzi, M.; Papaioannou, A.; Parenti, S.; Pariat, E.; Patsourakos, S.; Perrone, D.; Peter, H.; Pinto, R. F.; Plainaki, C.; Plettemeier, D.; Plunkett, S. P.; Raines, J. M.; Raouafi, N.; Reid, H.; Retino, A.; Rezeau, L.; Rochus, P.; Rodriguez, L.; Rodriguez-Garcia, L.; Roth, M.; Rouillard, A. P.; Sahraoui, F.; Sasso, C.; Schou, J.; Schühle, U.; Sorriso-Valvo, L.; Soucek, J.; Spadaro, D.; Stangalini, M.; Stansby, D.; Steller, M.; Strugarek, A.; Štverák, Š.; Susino, R.; Telloni, D.; Terasa, C.; Teriaca, L.; Toledo-Redondo, S.; del Toro Iniesta, J. C.; Tsiropoula, G.; Tsounis, A.; Tziotziou, K.; Valentini, F.; Vaivads, A.; Vecchio, A.; Velli, M.; Verbeeck, C.; Verdini, A.; Verscharen, D.; Vilmer, N.; Vourlidas, A.; Wicks, R.; Wimmer-Schweingruber, R. F.; Wiegelmann, T.; Young, P. R.; Zhukov, A. N., Solar Orbiter is the first space mission observing the solar plasma both in situ and remotely, from a close distance, in and out of the ecliptic. The ultimate goal is to understand how the Sun produces and controls the heliosphere, filling the Solar System and driving the planetary environments. With six remote-sensing and four in-situ instrument suites, the coordination and planning of the operations are essential to address the following four top-level science questions: (1) What drives the solar wind and where does the coronal magnetic field originate?; (2) How do solar transients drive heliospheric variability?; (3) How do solar eruptions produce energetic particle radiation that fills the heliosphere?; (4) How does the solar dynamo work and drive connections between the Sun and the heliosphere? Maximising the mission's science return requires considering the characteristics of each orbit, including the relative position of the spacecraft to Earth (affecting downlink rates), trajectory events (such as gravitational assist manoeuvres), and the phase of the solar activity cycle. Furthermore, since each orbit's science telemetry will be downloaded over the course of the following orbit, science operations must be planned at mission level, rather than at the level of individual orbits. It is important to explore the way in which those science questions are translated into an actual plan of observations that fits into the mission, thus ensuring that no opportunities are missed. First, the overarching goals are broken down into specific, answerable questions along with the required observations and the so-called Science Activity Plan (SAP) is developed to achieve this. The SAP groups objectives that require similar observations into Solar Orbiter Observing Plans, resulting in a strategic, top-level view of the optimal opportunities for science observations during the mission lifetime. This allows for all four mission goals to be addressed. In this paper, we introduce Solar Orbiter's SAP through a series of examples and the strategy being followed. © 2020 ESO., Solar Orbiter is a space mission of international collaboration between ESA and NASA with contributions from national agencies of ESA member states. The spacecraft has been developed by Airbus and is being operated by ESA from the European Space Operations Centre (ESOC) in Darmstadt, Germany. Science operations are carried out at ESA's European Space Astronomy Centre (ESAC) in Villafranca del Castillo, Spain. SWA is an international collaboration which has been funded by the UKSA, CNES, ASI, NASA and the Czech contribution to the ESA PRODEX programme. UAH authors want to thanks the Spanish MINECO-FPI-2016 predoctoral grant with FSE, and its project FEDER/MCIU-AEEI/Proyecto ESP2017-88436-R. The Spanish contribution to SO/PHI has been funded by the Spanish Ministry of Science and Innovation through several projects, the last one being RTI2018-096886-B-C5, and by "Centro de Excelencia Severo Ochoa" programme under grant SEV-2017-0709. RAH, RCC, DMM, SPP, and AV acknowledge the support of the NASA Heliophysics Division, Solar Orbiter Collaboration Office under IAT NNG09EK11I. JEP acknowledges grant UKRI/STFC ST/N000692/1. All French involvements are supported by CNES and CNRS. DV is supported by the STFC Ernest Rutherford Fellowship ST/P003826/1 and STFC Consolidated Grant ST/S000240/1. The authors thank the referee for her constructive comments and suggestions, which led to the substantial improvement of this paper.
Published: 2020

23. The RPW Low Frequency Receiver (LFR) on Solar Orbiter: in-situ LF electric and magnetic field measurements of the solar wind expansion

Author: Thomas Chust, Olivier Le Contel, Matthieu Berthomier, Alessandro Retinò, Fouad Sahraoui, Alexis Jeandet, Paul Leroy, Jean-Christophe Pellion, Bouzid, V., Bruno Katra, Rodrigue Piberne, Yuri Khotyaintsev, Andris Vaivads, Volodya Krasnoselskikh, Matthieu Kretzschmar, Jan Souček, Ondrej Santolík, Milan Maksimovic, Bale, Stuart D., Laboratoire de Physique des Plasmas (LPP), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École polytechnique (X)-Sorbonne Université (SU)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Observatoire de Paris, Swedish Institute of Space Physics [Kiruna] (IRF), 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), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2020

24. The RPW Time Domain Sampler (TDS) on Solar Orbiter: In-flight performance and first data

Author: Jan Soucek, Ludek Uhlir, Radek Lan, David Pisa, Ivana Kolmasova, Ondrej Santolik, Vratislav Krupar, Oksana Kruparova, Milan Maksimovic, Matthieu Kretzschmar, Yuri Khotyaintsev, and Thomas Chust
Subjects: Physics::Space Physics
Abstract: The Radio and Plasma Wave instrument (RPW) for Solar Orbiter includes a Time Domain Sampler sub-unit (TDS) designed to capture electromagnetic waveform measurements of high-frequency plasma waves and antenna voltage spikes associated with dust impacts. TDS will digitize three components of the electric field and one magnetic component at 524 kHz sampling rate and scan the obtained signal for plasma waves and dust impact signatures. The main science target of TDS are Langmuir waves observed in the solar wind in association with Type II and Type III solar bursts, interplanetary shocks, magnetic holes, and other phenomena. In this poster, we present the scientific data products provided by the TDS instrument and discuss the first data obtained during the commissioning phase. The first data will be used to evaluate the actual performance of the RPW TDS instrument.
Published: 2020

25. Initial in-flight performance results from Solar Orbiter RPW/BIAS

Author: Yuri V. Khotyaintsev, Andris Vaivads, Daniel B. Graham, Niklas J. T. Edberg, Erik P. G. Johansson, Milan Maksimovic, Stuart D. Bale, Thomas Chust, Matthieu Kretzschmar, and Jan Soucek
Abstract: The BIAS subsystem is a part of the Radio and Plasma Waves (RPW) instrument on the ESA Solar Orbiter mission. It allows sending bias current to each of the three RPW antennas. By setting the appropriate bias current the antenna potential can be shifted closer to the local plasma potential. This allows us to measure the floating potential of the spacecraft, as well as the electric field in the DC/LF frequency range with higher accuracy and lower noise level. Here we present the very initial results on RPW/BIAS in-flight performance based on the operations during the instrument commissioning.
Published: 2020

26. The Radio and Plasma Waves (RPW) Instrument on Solar Orbiter : Capabilities, Performance and First results

Author: Thomas Chust, Yuri V. Khotyaintsev, Xavier Bonnin, Matthieu Kretzschmar, M. Steller, Štěpán Štverák, Dirk Plettemeier, Stuart D. Bale, Jan Soucek, and Milan Maksimovic
Subjects: Physics, Orbiter, business.industry, law, Plasma, Aerospace engineering, business, law.invention
Abstract: We will review the instrumental capabilities of the Radio and Plasma Waves (RPW) Instrument on Solar Orbiter which at the time of writing this abstract is planned for a launch on February 5th 2020. This instrument is designed to measure in-situ magnetic and electric fields and waves from 'DC' to a few hundreds of kHz. RPW will also observe solar radio emissions up to 16 MHz. The RPW instrument is of primary importance to the Solar Orbiter mission and science requirements, since it is essential to answer three of the four mission overarching science objectives. In addition, RPW will exchange on-board data with the other in-situ instruments, in order to process algorithms for interplanetary shocks and type III Langmuir waves detections. If everything goes well after the launch, we will hopefully be able to present the first RPW data and results gathered during the commissioning.
Published: 2020

27. An Empirical Model of the Variation of the Solar Lyman‐ α Spectral Irradiance

Author: Martin Snow, Matthieu Kretzschmar, Werner Curdt, 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Max-Planck-Institut für Sonnensystemforschung (MPS), and Max-Planck-Gesellschaft
Subjects: Physics, 010504 meteorology & atmospheric sciences, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Irradiance, Solar cycle 23, Interplanetary medium, Lyman-alpha line, Astrophysics, Solar irradiance, 01 natural sciences, 7. Clean energy, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], Geophysics, 0103 physical sciences, General Earth and Planetary Sciences, Solstice, Variation (astronomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Solar variation
Abstract: International audience; We propose a simple model that computes the spectral profile of the solar irradiance in the hydrogen Lyman alpha line, H Ly-α(121.567nm), from 1947 to present. Such a model is relevant for the study of many astronomical environments, from planetary atmospheres to interplanetary medium. This empirical model is based on the SOHO/SUMER observations of the Ly-α irradiance over Solar Cycle 23 and the Ly-α disk-integrated irradiance composite. The model reproduces the temporal variability of the spectral profile and matches the independent SORCE/SOLSTICE spectral observations from 2003 to 2007 with an accuracy better than 10%.
Published: 2018

28. First Detection of Solar Flare Emission in Mid-ultraviolet Balmer Continuum

Author: Laurence Wauters, Werner Schmutz, Marie Dominique, Ingolf Dammasch, Matthieu Kretzschmar, Petr Heinzel, S. V. Shestov, L. Dolla, Andrei Zhukov, Giovanni Lapenta, Janet Machol, Solar-Terrestrial Centre of Excellence [Brussels] (STCE), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), 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, and 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)
Subjects: IMAGING-SPECTROGRAPH IRIS, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Continuum (design consultancy), MODELS, FOS: Physical sciences, chromosphere [Sun], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, WHITE-LIGHT FLARE, medicine.disease_cause, 01 natural sciences, REGION, symbols.namesake, 0103 physical sciences, medicine, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, UV radiation [Sun], SPECTRUM, Science & Technology, Solar flare, SUN, Balmer series, Astronomy and Astrophysics, PERFORMANCE, PROBA2, flares [Sun], RADIOMETER, Astrophysics - Solar and Stellar Astrophysics, RESOLUTION, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Physical Sciences, symbols, Ultraviolet
Abstract: © 2018. The American Astronomical Society. All rights reserved. We present the first detection of solar flare emission at mid-ultraviolet wavelengths around 2000 by the channel 2 of the Large-Yield RAdiometer (LYRA) on board the PRoject for OnBoard Autonomy 2 mission. The flare (SOL20170906) was also observed in the channel 1 of LYRA centered at the H i Ly line at 1216 showing a clear non-thermal profile in both channels. The flare radiation in channel 2 is consistent with the hydrogen Balmer continuum emission produced by an optically thin chromospheric slab heated up to 10,000 K. Simultaneous observations in channels 1 and 2 allow the separation of the line emission (primarily from the Ly line) from the Balmer continuum emission. Together with the recent detection of the Balmer continuum emission in the near-ultraviolet by the Interface Region Imaging Spectrometer, the LYRA observations strengthen the interpretation of broadband flare emission as the hydrogen recombination continua originating in the chromosphere. ispartof: ASTROPHYSICAL JOURNAL LETTERS vol:867 issue:2 status: published
Published: 2018

29. Temperature Dependence of the Flare Fluence Scaling Exponent

Author: Matthieu Kretzschmar, 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), European Project: 313188,EC:FP7:SPA,FP7-SPACE-2012-1,SOLID(2012), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (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 Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Physics, Solar flare, Flares, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, in flares, Solar irradiance, Fluence, Corona, law.invention, Heating, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, law, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Chromosphere, Scaling, Noise (radio), Flare
Abstract: International audience; Solar flares result in an increase of the solar irradiance at all wavelengths. While the distribution of the flare fluence observed in coronal emission has been widely studied and found to scale as , with slightly below 2, the distribution of the flare fluence in chromospheric lines is poorly known. We used the solar irradiance measurements observed by the SDO/EVE instrument at a 10 s cadence to investigate the dependency of the scaling exponent on the formation region of the lines (or temperature). We analyzed all flares above the C1 level since the start of the EVE observations (May 2010) to determine the flare fluence distribution in 16 lines covering a wide range of temperatures, several of which were not studied before. Our results show a weak downward trend with temperature of the scaling exponent of the PDF that reaches from above 2 at lower temperature (a few ) to for hot coronal emission (several ). However, because colder lines also have fainter contrast, we cannot exclude that this behavior is caused by including more noise for smaller flares for these lines. We discuss the method and its limitations and tentatively associate this possible trend with the different mechanisms responsible for the heating of the chromosphere and corona during flares.
Published: 2015

30. Where does the Thermospheric Ionospheric GEospheric Research (TIGER) Program go?

Author: Jens Berdermann, Gaël Cessateur, Ch. Jacobi, L. Ciraolo, Gerhard Schmidtke, R. Hammer, W. K. Tobiska, Alexander Gottwald, Stanley C. Solomon, Robert Schäfer, Wolfgang Schmidt, S.V. Avakyan, Sandro M. Radicella, Norbert Jakowski, Volker Bothmer, Matthieu Kretzschmar, Gérard Thuillier, Thierry Dudok de Wit, Seth Wieman, Thomas N. Woods, Francis G. Eparvier, Leonid Didkovsky, Marcel Pfeifer, Jean Lilensten, M. Haberreiter, Publica, Fraunhofer-Institut für Physikalische Messtechnik (Fraunhofer IPM), S.I. Vavilov State Optical Institute, DLR Institute of Communications and Navigation [Neustrelitz], German Aerospace Center (DLR), Georg-August-University [Göttingen], Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Abdus Salam International Centre for Theoretical Physics [Trieste] (ICTP), University of Southern California (USC), 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, 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)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Physikalisch-Technische Bundesanstalt [Berlin] (PTB), Kiepenheuer-Institut für Sonnenphysik (KIS), Universität Leipzig [Leipzig], 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), High Altitude Observatory (HAO), National Center for Atmospheric Research [Boulder] (NCAR), STRATO - 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), Space Environment, Technologies, Pacific Palisades, European Project: 313188,EC:FP7:SPA,FP7-SPACE-2012-1,SOLID(2012), Fraunhofer Institute for Physical Measurement Techniques (Fraunhofer IPM), Fraunhofer (Fraunhofer-Gesellschaft), Georg-August-University = Georg-August-Universität Göttingen, 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), Universität Leipzig, 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), Space Environment, Technologies [Pacific Palisades], Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and 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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])
Subjects: UV/EUV solar spectral irradiance, [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Atmospheric Science, Committee on Space Research, Total electron content, Meteorology, Modeling, Irradiance, Aerospace Engineering, Astronomy and Astrophysics, Space weather, Solar physics, Solar irradiance, 7. Clean energy, Geophysics, 13. Climate action, Space and Planetary Science, Extreme ultraviolet, Calibration, General Earth and Planetary Sciences, Environmental science, UV / EUV Solar Spectral Irradiance, Ionosphere, Instrumentation, Remote sensing
Abstract: International audience; At the 10th Thermospheric Ionospheric GEospheric Research (TIGER/COSPAR) symposium held in Moscow in 2014 the achievements from the start of TIGER in 1998 were summarized. During that period, great progress was made in measuring, understanding, and modeling the highly variable UV-Soft X-ray (XUV) solar spectral irradiance (SSI), and its effects on the upper atmosphere. However, after more than 50 years of work the radiometric accuracy of SSI observation is still an issue and requires further improvement. Based on the extreme ultraviolet (EUV) data from the SOLAR/SolACES, and SDO/EVE instruments, we present a combined data set for the spectral range from 16.5 to 105.5 nm covering a period of 3.5 years from 2011 through mid of 2014. This data set is used in ionospheric modeling of the global total electron content (TEC), and in validating EUV SSI modeling. For further investigations the period of 3.5 years is being extended to about 12 years by including data from SOHO/SEM and TIMED/SEE instruments. Similarly, UV data are used in modeling activities. After summarizing the results, concepts are proposed for future real-time SSI measurements with in-flight calibration as experienced with the ISS SOLAR payload, for the development of a space weather camera for observing and investigating space weather phenomena in real-time, and for providing data sets for SSI and climate modeling. Other planned topics are the investigation of the relationship between solar EUV/UV and visible/near-infrared emissions, the impact of X-rays on the upper atmosphere, the development of solar EUV/UV indices for different applications, and establishing a shared TIGER data system for EUV/UV SSI data distribution and real-time streaming, also taking into account the achievements of the FP7 SOLID (First European SOLar Irradiance Data Exploitation) project. - For further progress it is imperative that coordinating activities in this special field of solar-terrestrial relations and solar physics is emphasized.
Published: 2015

31. Global Energetics of Solar Flares: V. Energy Closure in Flares and Coronal Mass Ejections

Author: Gordon D. Holman, Matthieu Kretzschmar, R. A. Mewaldt, Yan Xu, Ju Jing, Eduard P. Kontar, Amir Caspi, Harry P. Warren, James M. McTiernan, Daniel F. Ryan, Christina Cohen, Markus J. Aschwanden, Aidan M. O'Flannagain, and Ian G. Richardson
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Electron, 7. Clean energy, 01 natural sciences, law.invention, Luminosity, Ion, law, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Solar flare, business.industry, Astronomy and Astrophysics, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Energy (signal processing), Thermal energy, Flare
Abstract: In this study we synthesize the results of four previous studies on the global energetics of solar flares and associated coronal mass ejections (CMEs), which include magnetic, thermal, nonthermal, and CME energies in 399 solar M and X-class flare events observed during the first 3.5 years of the Solar Dynamics Observatory (SDO) mission. Our findings are: (1) The sum of the mean nonthermal energy of flare-accelerated particles ($E_{\mathrm{nt}}$), the energy of direct heating ($E_{\mathrm{dir}}$), and the energy in coronal mass ejections ($E_{\mathrm{CME}}$), which are the primary energy dissipation processes in a flare, is found to have a ratio of $(E_{\mathrm{nt}}+E_{\mathrm{dir}}+ E_{\mathrm{CME}})/E_{\mathrm{mag}} = 0.87 \pm 0.18$, compared with the dissipated magnetic free energy $E_{\mathrm{mag}}$, which confirms energy closure within the measurement uncertainties and corroborates the magnetic origin of flares and CMEs; (2) The energy partition of the dissipated magnetic free energy is: $0.51\pm0.17$ in nonthermal energy of $\ge 6$ keV electrons, $0.17\pm0.17$ in nonthermal $\ge 1$ MeV ions, $0.07\pm0.14$ in CMEs, and $0.07\pm0.17$ in direct heating; (3) The thermal energy is almost always less than the nonthermal energy, which is consistent with the thick-target model; (4) The bolometric luminosity in white-light flares is comparable with the thermal energy in soft X-rays (SXR); (5) Solar Energetic Particle (SEP) events carry a fraction $\approx 0.03$ of the CME energy, which is consistent with CME-driven shock acceleration; and (6) The warm-target model predicts a lower limit of the low-energy cutoff at $e_c \approx 6$ keV, based on the mean differential emission measure (DEM) peak temperature of $T_e=8.6$ MK during flares. This work represents the first statistical study that establishes energy closure in solar flare/CME events., 35 pages, 10 Figures, accepted for publication in The Astrophysical Journal
Published: 2017

32. The LYRA Instrument Onboard PROBA2: Description and In-Flight Performance

Author: Ingolf Dammasch, Alexander Shapiro, Yvan Stockman, Andrei Zhukov, M. Dominique, Ali BenMoussa, Jean-François Hochedez, Matthieu Kretzschmar, Werner Schmutz, Didier Gillotay, Solar-Terrestrial Centre of Excellence [Brussels] (STCE), 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), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), D.V. Skobeltsyn Institute of Nuclear Physics (SINP), Lomonosov Moscow State University (MSU), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Centre Spatial de Liège (CSL), Université de Liège, Belgian Federal Science Policy Office through the ESA-PRODEX program, Belgian Federal Science Policy Offce (BELSPO), Swiss Bundesamt fur Bildung und Wissenschaft, 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, and 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)
Subjects: Eclipse observations, 010504 meteorology & atmospheric sciences, Data products, Computer science, FOS: Physical sciences, Space weather, Solar irradiance, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Instrumentation and data management, 0105 earth and related environmental sciences, Remote sensing, Radiometer, Flares, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Aeronomy, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Solar physics, Earth atmosphere, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: International audience; The Large Yield Radiometer (LYRA) is an XUV-EUV-MUV (soft X-ray to mid-ultraviolet) solar radiometer onboard the European Space Agency Project for On-Board Autonomy 2 (PROBA2) mission, which was launched in November 2009. LYRA acquires solar-irradiance measurements at a high cadence (nominally 20 Hz) in four broad spectral channels, from soft X-ray to MUV, which have been chosen for their relevance to solar physics, space weather, and aeronomy. We briefly review the design of the instrument, give an overview of the data products distributed through the instrument website, and describe how the data are calibrated. We also briefly present a summary of the main fields of research currently under investigation by the LYRA consortium.
Published: 2013

33. Response of the low ionosphere to X-ray and Lyman-α solar flare emissions

Author: Jean-Pierre Raulin, Matthieu Kretzschmar, Edith L. Macotela, Fernando C. P. Bertoni, Ingolf Dammasch, Gerard Trottet, and Alessandra Abe Pacini
Subjects: Solar minimum, Physics, 010504 meteorology & atmospheric sciences, Solar flare, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Solar cycle 22, Astrophysics::Cosmology and Extragalactic Astrophysics, Solar maximum, 01 natural sciences, Physics::Geophysics, Solar cycle, Geophysics, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Very low frequency, Ionosphere, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: [1] Using soft X-ray measurements from detectors onboard the Geostationary Operational Environmental Satellite (GOES) and simultaneous high-cadence Lyman-a observations from the Large Yield Radiometer (LYRA) onboard the Project for On-Board Autonomy 2 (PROBA2) ESA spacecraft, we study the response of the lower part of the ionosphere, the D region, to seven moderate to medium-size solar flares that occurred in February and March of 2010. The ionospheric disturbances are analyzed by monitoring the resulting sub-ionospheric wave propagation anomalies detected by the South America Very Low Frequency (VLF) Network (SAVNET). We find that the ionospheric disturbances, which are characterized by changes of the VLF wave phase, do not depend on the presence of Lyman-a radiation excesses during the flares. Indeed, Lyman-a excesses associated with flares do not produce measurable phase changes. Our results are in agreement with what is expected in terms of forcing of the lower ionosphere by quiescent Lyman-a emission along the solar activity cycle. Therefore, while phase changes using the VLF technique may be a good indicator of quiescent Lyman-a variations along the solar cycle, they cannot be used to scale explosive Lyman-a emission during flares.
Published: 2013

34. On-Orbit Degradation of Solar Instruments

Author: Vincenzo Andretta, Udo Schühle, D. Walton, C. Jeppesen, L. Bradley, Matthieu Kretzschmar, M. Dominique, Abdanour Irbah, Andrew R. Jones, Thomas N. Woods, B. Giordanengo, C. J. Eyles, Werner Schmutz, G. Del Zanna, Gregory J. Ucker, Frédéric Auchère, Francis G. Eparvier, Daniel B. Seaton, Daniel Stephen Brown, Leonid Didkovsky, Don Woodraska, Seth Wieman, Darrell L. Judge, Jean-Philippe Halain, David Berghmans, Mustapha Meftah, Thomas Foujols, S. Mekaoui, Gaël Cessateur, G. Thuillier, Steven Dewitte, I. E. Dammasch, Rachel Hock, D. Gillotay, B. Nicula, Phillip C. Chamberlin, Samuel Gissot, Ali BenMoussa, David Bolsee, Danielle Bewsher, D. R. McMullin, Solar-Terrestrial Centre of Excellence [Brussels] (STCE), Royal Observatory of Belgium [Brussels] (ROB), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Department of Applied Mathematics and Theoretical Physics (DAMTP), University of Cambridge [UK] (CAM), 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), Institut Royal Météorologique de Belgique [Bruxelles] (IRM), European Commission - Joint Research Centre [Ispra] (JRC), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Grupo de Astronomia y Ciencias del Espacio (GACE), Laboratorio de Procesado de Imagenes [Valencia] (LPI), Universitat de València (UV)-Universitat de València (UV), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), STRATO - 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), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), NASA Goddard Space Flight Center (GSFC), University of Southern California (USC), 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), Centre Spatial de Liège (CSL), Université de Liège, Air Force Research Laboratory (AFRL), United States Air Force (USAF), 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Space Systems Research Corporation (SSRC), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), 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 Royal Météorologique de Belgique [Bruxelles] - Royal Meteorological Institute (IRM), 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, and 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)
Subjects: solar instruments, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Solar mission, Space weather, Space (commercial competition), 7. Clean energy, 01 natural sciences, Space exploration, Degradation, Contamination, Observatory, 0103 physical sciences, Aerospace engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, business.industry, Astronomy and Astrophysics, con- tamination, calibration, space environment, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Orbit (dynamics), Environmental science, Astrophysics - Instrumentation and Methods for Astrophysics, business, Space environment, Degradation (telecommunications)
Abstract: International audience; We present the lessons learned about the degradation observed in several space solar missions, based on contributions at the Workshop about On-Orbit Degradation of Solar and Space Weather Instruments that took place at the Solar Terrestrial Centre of Excellence (Royal Observatory of Belgium) in Brussels on 3 May 2012. The aim of this workshop was to open discussions related to the degradation observed in Sun-observing instruments exposed to the effects of the space environment. This article summarizes the various lessons learned and offers recommendations to reduce or correct expected degradation with the goal of increasing the useful lifespan of future and ongoing space missions.
Published: 2013
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35. Making of a solar spectral irradiance dataset I: observations, uncertainties, and methods

Author: Margit Haberreiter, Matthieu Kretzschmar, Micha Schöll, Thierry Dudok de Wit, 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), European Project: 313188,EC:FP7:SPA,FP7-SPACE-2012-1,SOLID(2012), 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, and 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)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Computer science, Irradiance, Data analysis, Time series analysis, [SDU.STU.ME]Sciences of the Universe [physics]/Earth Sciences/Meteorology, lcsh:QC851-999, Solar irradiance, 7. Clean energy, 01 natural sciences, Proxy (climate), 0103 physical sciences, Statistics and probability, Time series, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Missing data, Autoregressive model, Solar spectrum, 13. Climate action, Space and Planetary Science, Outlier, Anomaly detection, lcsh:Meteorology. Climatology, Algorithms
Abstract: Context. Changes in the spectral solar irradiance (SSI) are a key driver of the variability of the Earth’s environment, strongly affecting the upper atmosphere, but also impacting climate. However, its measurements have been sparse and of different quality. The “First European Comprehensive Solar Irradiance Data Exploitation project” (SOLID) aims at merging the complete set of European irradiance data, complemented by archive data that include data from non-European missions. Aims. As part of SOLID, we present all available space-based SSI measurements, reference spectra, and relevant proxies in a unified format with regular temporal re-gridding, interpolation, gap-filling as well as associated uncertainty estimations. Methods. We apply a coherent methodology to all available SSI datasets. Our pipeline approach consists of the pre-processing of the data, the interpolation of missing data by utilizing the spectral coherency of SSI, the temporal re-gridding of the data, an instrumental outlier detection routine, and a proxy-based interpolation for missing and flagged values. In particular, to detect instrumental outliers, we combine an autoregressive model with proxy data. We independently estimate the precision and stability of each individual dataset and flag all changes due to processing in an accompanying quality mask. Results. We present a unified database of solar activity records with accompanying meta-data and uncertainties. Conclusions. This dataset can be used for further investigations of the long-term trend of solar activity and the construction of a homogeneous SSI record.
Published: 2016

36. Fast and robust segmentation of solar EUV images: algorithm and results for solar cycle 23

Author: Jean-François Hochedez, Véronique Delouille, Vincent Barra, Matthieu Kretzschmar, Laboratoire d'Informatique, de Modélisation et d'optimisation des Systèmes (LIMOS), SIGMA Clermont (SIGMA Clermont)-Université d'Auvergne - Clermont-Ferrand I (UdA)-Ecole Nationale Supérieure des Mines de St Etienne-Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP), Royal Observatory of Belgium [Brussels] (ROB), 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Université d'Auvergne - Clermont-Ferrand I (UdA)-SIGMA Clermont (SIGMA Clermont)-Ecole Nationale Supérieure des Mines de St Etienne (ENSM ST-ETIENNE)-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)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Fuzzy clustering, 010504 meteorology & atmospheric sciences, Solar cycle 23, Coronal hole, techniques: image processing, Space weather, Solar irradiance, 01 natural sciences, Sun: activity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Cluster analysis, 010303 astronomy & astrophysics, Sun: rotation, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Sun: corona, Astronomy and Astrophysics, Sun: UV radiation, Solar cycle, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Physics::Space Physics, Solar rotation, Algorithm
Abstract: International audience; Context. The study of the variability of the solar corona and the monitoring of coronal holes, quiet sun and active regions are of great importance in astrophysics as well as for space weather and space climate applications. Aims. In a previous work, we presented the spatial possibilistic clustering algorithm (SPoCA). This is a multi-channel unsupervised spatially-constrained fuzzy clustering method that automatically segments solar extreme ultraviolet (EUV) images into regions of interest. The results we reported on SoHO-EIT images taken from February 1997 to May 2005 were consistent with previous knowledge in terms of both areas and intensity estimations. However, they presented some artifacts due to the method itself. Methods. Herein, we propose a new algorithm, based on SPoCA, that removes these artifacts. We focus on two points: the definition of an optimal clustering with respect to the regions of interest, and the accurate definition of the cluster edges. We moreover propose methodological extensions to this method, and we illustrate these extensions with the automatic tracking of active regions. Results. The much improved algorithm can decompose the whole set of EIT solar images over the 23rd solar cycle into regions that can clearly be identified as quiet sun, coronal hole and active region. The variations of the parameters resulting from the segmentation, i.e. the area, mean intensity, and relative contribution to the solar irradiance, are consistent with previous results and thus validate the decomposition. Furthermore, we find indications for a small variation of the mean intensity of each region in correlation with the solar cycle. Conclusions. The method is generic enough to allow the introduction of other channels or data. New applications are now expected, e.g. related to SDO-AIA data.
Published: 2009

37. Review on the solar spectral variability in the EUV for space weather purposes

Author: J. Aboudarham, Pierre-Olivier Amblard, Matthieu Kretzschmar, Saïd Moussaoui, T. Dudok de Wit, Jean Lilensten, Frédéric Auchère, 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), Université Joseph Fourier - Grenoble 1 (UJF), 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), Solar Influences Data Analysis Center [Brussels] (SIDC), Royal Observatory of Belgium [Brussels] (ROB), GIPSA - Signal Images Physique (GIPSA-SIGMAPHY), Département Images et Signal (GIPSA-DIS), Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche en Communication et Cybernétique de Nantes, 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 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)-Centre National d’Études Spatiales [Paris] (CNES), Université Stendhal - Grenoble 3-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Stendhal - Grenoble 3-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Stendhal - Grenoble 3-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Stendhal - Grenoble 3-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Nowcasting, Meteorology, radiation and cosmic ray effects) – Solar physics, Flux, Space weather, Solar, 01 natural sciences, 7. Clean energy, Ultraviolet astronomy, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Astrophysics::Solar and Stellar Astrophysics, lcsh:Science, 010303 astronomy & astrophysics, Ionosphere (Modeling and forecasting, astronomy (Ultraviolet emissions), Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], lcsh:QC801-809, Geology, Astronomy and Astrophysics, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph], lcsh:QC1-999, lcsh:Geophysics. Cosmic physics, 13. Climate action, Space and Planetary Science, Physics::Space Physics, lcsh:Q, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Thermosphere, Energy source, physics, lcsh:Physics, Space environment, astro
Abstract: The solar XUV-EUV flux is the main energy source in the terrestrial diurnal thermosphere: it produces ionization, dissociation, excitation and heating. Accurate knowledge of this flux is of prime importance for space weather. We first list the space weather applications that require nowcasting and forecasting of the solar XUV-EUV flux. We then review present models and discuss how they account for the variability of the solar spectrum. We show why the measurement of the full spectrum is difficult, and why it is illusory to retrieve it from its atmospheric effects. We then address the problem of determining a set of observations that are adapted for space weather purposes, in the frame of ionospheric studies. Finally, we review the existing and future space experiments that are devoted to the observation of the solar XUV-EUV spectrum.
Published: 2008

38. Thermodynamics of rare events and impulsive relaxation events in the magnetospheric substorm dynamics

Author: Matthieu Kretzschmar and Giuseppe Consolini
Subjects: Physics, Space and Planetary Science, Turbulence, Physics::Space Physics, Substorm, Dynamics (mechanics), Rare events, Magnetosphere, Relaxation (physics), Thermodynamics, Astronomy and Astrophysics, Observable
Abstract: The magnetosphere dynamics shows fast relaxation events following power-law distribution for many observable quantities during magnetic substorms. The emergence of such power-law distributions has been widely discussed in the framework of self-organized criticality and/or turbulence. Here, a different approach to the statistical features of these impulsive dynamical events is proposed in the framework of the thermodynamics of rare events [Lavenda, B.H., Florio, A., 1992. Thermodynamics of rare events, Int. J. Theor. Phys. 31, 1455–1475; Lavenda, B.H., 1995. Thermodynamics of Extremes. Albion]. In detail, an application of such a novel approach to the magnetospheric substorm avalanching dynamics as monitored by the auroral electroject index is discussed.
Published: 2007

39. Recommendation for a set of solar EUV lines to be monitored for aeronomy applications

Author: Matthieu Kretzschmar, T. Dudok de Wit, Jean Lilensten, J. Aboudarham, Frédéric Auchère, Pierre-Olivier Amblard, 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), 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), GIPSA - Signal Images Physique (GIPSA-SIGMAPHY), Département Images et Signal (GIPSA-DIS), Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Grenoble Images Parole Signal Automatique (GIPSA-lab), Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Pierre Mendès France - Grenoble 2 (UPMF)-Université Stendhal - Grenoble 3-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), 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, 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), 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), SIDC, Royal Observatory of Belgium [Brussels] (ROB), Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-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, 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 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)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Extreme ultraviolet lithography, [SDE.MCG]Environmental Sciences/Global Changes, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], 01 natural sciences, Spectral line, Set (abstract data type), Optics, [INFO.INFO-TS]Computer Science [cs]/Signal and Image Processing, Ultraviolet astronomy, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), lcsh:Science, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, business.industry, Solar spectra, Aeronomy, lcsh:QC801-809, Geology, Astronomy and Astrophysics, lcsh:QC1-999, lcsh:Geophysics. Cosmic physics, Space and Planetary Science, Line (geometry), lcsh:Q, Ionosphere, business, [SPI.SIGNAL]Engineering Sciences [physics]/Signal and Image processing, lcsh:Physics
Abstract: In two recent studies, Dudok de Wit et al. (2005) and Kretzschmar et al. (2006) have shown that the solar Ultra-Violet spectrum between 25 and 195 nm can be reconstructed from the observation of a set of 6 to 10 carefully chosen spectral lines. The best set of lines, however, is application dependent. In this study, we demonstrate that a good candidate for aeronomy applications consists of the following 6 lines: H I at 102.572 nm, C III at 97.702 nm, O V at 62.973 nm, He I at 58.433 nm, Fe XV at 28.415 nm and He II at 30.378 nm. The TRANSCAR model is used to quantify the impact of each individual line on the density, temperature and velocity profiles. Using a multidimensional scaling technique, we show how to select from this the best set of lines. Although this selection is motivated by the specification of the ionosphere, our set of lines is also found to be appropriate for reconstructing the variability of the solar spectrum between 25 and 195 nm.
Published: 2007

40. Solar Spectral Irradiance Observations from the PICARD/PREMOS Radiometer

Author: Micha Schöll, Gaël Cessateur, Werner Schmutz, Christoph Wehrli, Julian Groebner, Margit Haberreiter, Matthieu Kretzschmar, Alexander Shapiro, Gérard Thuillier, Wolfgang Finsterle, Nigel Fox, Jean-François Hochedez, Silvio Koller, Mustapha Meftah, Stephan Nyeki, Daniel Pfiffner, Hansjörg Roth, Michel Rouzé, Marcel Spescha, Rinat Tagirov, Lutz Werner, Jules Wyss, Cardon, Catherine, Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, STRATO - 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), National Physical Laboratory [Teddington] (NPL), Centre National d'Études Spatiales [Toulouse] (CNES), Physikalisch-Technische Bundesanstalt [Berlin] (PTB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), and Max-Planck-Institut für Sonnensystemforschung (MPS)
Subjects: [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
Abstract: International audience; Space weather and space climate studies require accurate Solar Spectral Irradiance (SSI) observations. The PREcision Monitoring Sensor (PREMOS) instrument aboard the PICARD satellite acquired solar irradiance measurements in specific spectral windows in the UV, visible and near infrared from October 2010 to March 2014. This contribution aims at presenting the Level 3 data, corrected for non solar features as well as for degradation. These level 3 data has been tested over different scientific cases, such as observations during the Venus transit and the presence of the p-mode signature within high-cadence data. The PREMOS Level 3 data have also been compared to others data sets, namely the SOLSTICE and SIM instruments aboard SORCE, for nearly 3 and half years. An excellent correlation has been found for the UV spectral ranges. We have also found a rather good correlation for visible and near-infrared observations for short-term variations, for which an error of about 200 ppm has been estimated within PREMOS visible and near-infrared observations. The PREMOS data could also be used to address several scientific topics, i.e. for validating semi-empirical models of the solar irradiance. We will emphasize about our new irradiance model, COSIR for Code of Solar Irradiance Reconstruction, which is successful at reproducing the solar modulation as seen in the PREMOS, SoHO/Virgo and SORCE data.
Published: 2015

41. A Thermodynamic Approach to the Magnetospheric Complexity: The Role of Fluctuations

Author: Paola De Michelis, Matthieu Kretzschmar, and Giuseppe Consolini
Subjects: Physics, Diffusion equation, Criticality, Diffusion process, Space and Planetary Science, Physics::Space Physics, Relaxation (physics), Astronomy and Astrophysics, Statistical physics, Diffusion (business), Convection–diffusion equation, Composite analysis
Abstract: Recent studies evidenced that the magnetotail dynamics looks like the one of an avalanching system. This fact has been related with a near criticality dynamics and modelled by singular diffusion and transport equations. Here, we discuss some features of the Earth’s magnetotail dynamics using a thermodynamic approach. In detail we discuss the role played by fluctuations in singular diffusion and relaxation processes from a non-equilibrium thermodynamics point of view. Moreover, the emergence of non-Gaussian statistics is discussed in the framework of the thermodynamics of composite systems.
Published: 2006

42. Retrieving the solar EUV spectral irradiance from the observation of 6 lines

Author: Matthieu Kretzschmar, J. Aboudarham, Jean Lilensten, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), 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), 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), Consiglio Nazionale delle Ricerche (CNR), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and 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)
Subjects: Physics::General Physics, Atmospheric Science, 010504 meteorology & atmospheric sciences, Differential emission measure, Extreme ultraviolet lithography, Irradiance, Aerospace Engineering, Solar irradiance, 7. Clean energy, 01 natural sciences, Solar EUV irradiance, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Physics, Astronomy, Astronomy and Astrophysics, Solar cycle, Geophysics, 13. Climate action, Space and Planetary Science, Extreme ultraviolet, Physics::Space Physics, General Earth and Planetary Sciences, Solar–terrestrial relationship, Astrophysics::Earth and Planetary Astrophysics, Ionosphere, Thermosphere
Abstract: International audience; We use recent solar extreme ultraviolet (EUV) irradiance data from the Solar EUV Experiment aboard the Thermosphere Ionosphere Mesosphere Energetics and Dynamics satellite to investigate the possibility to retrieve the whole solar EUV irradiance from a minimum number of measurements. Computing a differential emission measure for the whole Sun from the irradiances of 5 lines and using a sixth line to model optically thick emission, we are able to reproduce with a good agreement the variability of the whole solar EUV irradiance.
Published: 2006

43. Complexity in the Earth’s magnetotail plasma sheet

Author: Giuseppe Consolini and Matthieu Kretzschmar
Subjects: Physics, Atmospheric Science, Statistical pattern, Plasma sheet, Complex system, Aerospace Engineering, Astronomy and Astrophysics, Magnetic field, Nonlinear system, Geophysics, Classical mechanics, Space and Planetary Science, Physics::Space Physics, General Earth and Planetary Sciences, Statistical physics, Scaling, Randomness, Topology (chemistry)
Abstract: The Earth’s magnetotail plasma sheet acts as a reservoir of energy and particles for magnetospheric processes, and is now well recognized to behave as a nonlinear complex system. Several recent studies have provided strong evidence for the multiscale, cross-coupling, and re-organization processes in the magnetotail plasma sheet phenomena, suggesting that new approaches may be useful to provide new insight on the complex nature of the dynamics of this region. Here, after a brief review of some recent results on the complexity of plasma sheet dynamics, we discuss the relevance of randomness in the magnetic field fluctuations by means of simulated statistical pattern. In detail, we show how scale-invariance properties, which resemble actual measurement features, can be observed also in simple static random model. The results are also discussed in connection with a complex topology of the geotail currents.
Published: 2006

44. Variability of the EUV quiet Sun emission and reference spectrum using SUMER

Author: Jean Lilensten, Matthieu Kretzschmar, J. Aboudarham, 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), 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 solaire, 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: Physics, Space and Planetary Science, QUIET, Extreme ultraviolet lithography, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Large range, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Spectral line
Abstract: International audience; This paper aims to build a quiet Sun EUV reference spectrum from the SOHO - SUMER database. We make use of 750 quiet Sun spectra spread over a large range of solar activity. They are carefully calibrated both in terms of frequency and intensity. The data do not show any noticeable variations versus the solar activity. This allows us to build a quiet Sun reference spectrum from data scattered over any solar activity level. We consider separately the continuum, the thick-line spectra, and the thin-line spectra. The former is computed from an average of the H Lyman and C I continua. The thick lines are directly assembled from the SUMER files. To retrieve a broad set of thin lines, we use the SUMER measurements to compute a mean Differential Emission Measure, which is then inverted. This results in a reference spectrum for the Quiet Sun, which is compared to previous studies.
Published: 2004

45. Solar flares at submillimeter wavelengths

Author: Timothy S. Bastian, C. G. Giménez de Castro, Jana Kašparová, Antonio Hales, Alexander L. MacKinnon, Matthieu Kretzschmar, Säm Krucker, Karl-Ludwig Klein, T. Lüthi, Silja Pohjolainen, G. Trottet, Hugh S. Hudson, Stephen M. White, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, University of Applied Sciences Western Switzerland, 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, 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), Laboratoire d’Océanologie et de Géosciences (LOG) - UMR 8187 (LOG), Institut national des sciences de l'Univers (INSU - CNRS)-Université du Littoral Côte d'Opale (ULCO)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut of Physiology, Czech Academy of Sciences [Prague] (CAS), Monash University [Malaysia], 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Institute for Atmospheric and Climate Science [Zürich] (IAC), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Lawrence Livermore National Laboratory (LLNL), 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), Université de Lille-Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique (CNRS), Czech Academy of Sciences [Prague] (ASCR), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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 national des sciences de l'Univers (INSU - CNRS)-Université du Littoral Côte d'Opale (ULCO)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Nord]), 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), Université du Littoral Côte d'Opale-Université de Lille-Centre National de la Recherche Scientifique (CNRS), 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: Physics, Sun: flares, 010504 meteorology & atmospheric sciences, Solar flare, Terahertz radiation, Sun: radio observations, Flare star, Astronomy, Astronomy and Astrophysics, Astrophysics, Spectral component, 01 natural sciences, Spectral line, law.invention, Particle acceleration, Wavelength, Space and Planetary Science, law, [SDU]Sciences of the Universe [physics], 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Flare
Abstract: International audience; We discuss the implications of the first systematic observations of solar flares at submillimeter wavelengths, defined here as observing wavelengths shorter than 3 mm (frequencies higher than 0.1 THz). The events observed thus far show that this wave band requires a new understanding of high-energy processes in solar flares. Several events, including observations from two different observatories, show during the impulsive phase of the flare a spectral component with a positive (increasing) slope at the highest observable frequencies (up to 405 GHz). To emphasize the increasing spectra and the possibility that these events could be even more prominent in the THz range, we term this spectral feature a "THz component". Here we review the data and methods, and critically assess the observational evidence for such distinct component(s). This evidence is convincing. We also review the several proposed explanations for these feature(s), which have been reported in three distinct flare phases. These data contain important clues to flare development and particle acceleration as a whole, but many of the theoretical issues remain open. We generally have lacked systematic observations in the millimeter-wave to far-infrared range that are needed to complete our picture of these events, and encourage observations with new facilities.
Published: 2013

46. The Space Weather & Ultraviolet Solar Variability Microsatellite Mission (SWUSV)

Author: José M.G. Merayo, Alexander Shapiro, Slimane Bekki, R. Kariyappa, Mustapha Meftah, Vladimir Slemzin, Ayman Mahrous, Marion Marchand, Abdanour Irbah, Philippe Keckhut, Thomas Foujols, Antonis Paschalis, Besheir Marzouk, Eric Quémerais, Sergey S. Bogachev, Alain Hauchecorne, Ahmed Abdel Hady, Gaël Cessateur, Safinaz A. Khaled, Sergey Kuzin, Peter Brauer, Matthieu Kretzschmar, Alain Sarkissian, Ahmed Ghitas, Kanaris Tsinganos, Amal Zaki, Werner Schmutz, Luc Damé, 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), STRATO - 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), 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), Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Section of Astrophysics, Astronomy and Mechanics [Athens], National and Kapodistrian University of Athens (NKUA), Université d'Helwan, National Research Institute of Astronomy and Geophysics [Helwan] (NRIAG), National Authority for Remote Sensing and Space Sciences (NARSS), and Université d'Orléans (UO)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 0303 health sciences, Solar flare, solar flares, Payload, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, solar variability, Space weather, medicine.disease_cause, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrobiology, 03 medical and health sciences, 0302 clinical medicine, Space and Planetary Science, 030220 oncology & carcinogenesis, ultraviolet, medicine, Coronal mass ejection, Space Weather, Ultraviolet, Coronal Mass Ejections, 030304 developmental biology, Solar variation
Abstract: We present a summary of the scientific objectives, payload and mission profile of the Space Weather & Ultraviolet Solar Variability Microsatellite Mission (SWUSV) proposed to CNES and ESA (small mission).
Published: 2013

47. Coronal Temperature Maps from Solar EUV Images: A Blind Source Separation Approach

Author: T. Dudok de Wit, Gaël Cessateur, Saïd Moussaoui, Matthieu Kretzschmar, Chloé Guennou, Luis Eduardo Antunes Vieira, Frédéric Auchère, F. Goryaev, 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Recherche en Communications et en Cybernétique de Nantes (IRCCyN), Mines Nantes (Mines Nantes)-École Centrale de Nantes (ECN)-Ecole Polytechnique de l'Université de Nantes (EPUN), Université de Nantes (UN)-Université de Nantes (UN)-PRES Université Nantes Angers Le Mans (UNAM)-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), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), P. N. Lebedev Physical Institute of the Russian Academy of Sciences [Moscow] (LPI RAS), Russian Academy of Sciences [Moscow] (RAS), European Project: 218816,EC:FP7:SPA,FP7-SPACE-2007-1,SOTERIA(2008), 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), 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), and Institut national des sciences de l'Univers (INSU - CNRS)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Ultraviolet spectrum, 010504 meteorology & atmospheric sciences, Solar image processing, Extreme ultraviolet lithography, Bayesian inference, FOS: Physical sciences, Coronal hole, Solar corona, 01 natural sciences, 7. Clean energy, Blind signal separation, 0103 physical sciences, Range (statistics), Linear combination, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Spectral bands, Computational physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Extreme ultraviolet, Physics - Data Analysis, Statistics and Probability, Blind source separation, Data Analysis, Statistics and Probability (physics.data-an), Data reduction
Abstract: Multi-wavelength solar images in the EUV are routinely used for analysing solar features such as coronal holes, filaments, and flares. However, images taken in different bands often look remarkably similar as each band receives contributions coming from regions with a range of different temperatures. This has motivated the search for empirical techniques that may unmix these contributions and concentrate salient morphological features of the corona in a smaller set of less redundant source images. Blind Source Separation (BSS) precisely does this. Here we show how this novel concept also provides new insight into the physics of the solar corona, using observations made by SDO/AIA. The source images are extracted using a Bayesian positive source separation technique. We show how observations made in six spectral bands, corresponding to optically thin emissions, can be reconstructed by linear combination of three sources. These sources have a narrower temperature response and allow for considerable data reduction since the pertinent information from all six bands can be condensed in only one single composite picture. In addition, they give access to empirical temperature maps of the corona. The limitations of the BSS technique and some applications are briefly discussed., to appear in Solar Physics (2012)
Published: 2013

48. Solar activity and its evolution across the corona: recent advances

Author: Laura A. Balmaceda, Marilena Mierla, Rami Vainio, Jens Pomoell, Jean Lilensten, Thierry Dudok de Wit, Gaël Cessateur, Francesca Zuccarello, Susanna Parenti, Fernando M. López, Matthieu Kretzschmar, Francesco Zuccarello, Matthew J. West, Salvatore Luigi Guglielmino, Paolo Romano, Hebe Cremades, Nandita Srivastava, Luciano Rodriguez, 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), Instituto de Ciencias Astronómicas, de la Tierra y del Espacio [San Juan] (ICATE), Facultad de Ciencias Exactas, Físicas y Naturales [San Juan] (FCEFN), Universidad Nacional de San Juan (UNSJ)-Universidad Nacional de San Juan (UNSJ), Centre de Recherche en Astronomie Astrophysique et Géophysique (CRAAG), Facultad Regional Mendoza (FRM), Universidad Tecnológica Nacional [Sarmiento] (UTN), Osservatorio Astrofisico di Catania, Istituto Nazionale di Astrofisica (INAF), 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), 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)-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, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Solar Influences Data Analysis Center [Brussels] (SIDC), Royal Observatory of Belgium [Brussels], Department of Engineering Physics, Helsinki University of Technology, PO Box 4100, FI-02015 HUT, FINLAND, Udaipur Solar Observatory, Physical Research Laboratory [Ahmedabad] (PRL), Indian Space Research Organisation (ISRO)-Indian Space Research Organisation (ISRO), Centre for Mathematical Plasma-Astrophysics [Leuven] (CmPA), Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), 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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-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 de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Royal Observatory of Belgium [Brussels] (ROB), 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), Universidad Nacional de San Juan [Argentine] (UNSJ)-Universidad Nacional de San Juan [Argentine] (UNSJ), 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), 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, and 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)
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Ciencias Físicas, Space weather, Solar irradiance, 01 natural sciences, 7. Clean energy, Solar prominence, purl.org/becyt/ford/1 [https], Meteorology. Climatology, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, Cost action, Interplanetary magnetic field, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, coronal mass ejections, Physics, active regions, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy, solar irradiance, purl.org/becyt/ford/1.3 [https], Solar atmosphere, Wide field, Astronomía, 13. Climate action, Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, shock propagation, QC851-999, solar activity, CIENCIAS NATURALES Y EXACTAS
Abstract: Solar magnetism is responsible for the several active phenomena that occur in the solar atmosphere. The consequences of these phenomena on the solar-terrestrial environment and on Space Weather are nowadays clearly recognized, even if not yet fully understood. In order to shed light on the mechanisms that are at the basis of the Space Weather, it is necessary to investigate the sequence of phenomena starting in the solar atmosphere and developing across the outer layers of the Sun and along the path from the Sun to the Earth. This goal can be reached by a combined multi-disciplinary, multi-instrument, multi-wavelength study of these phenomena, starting with the very first manifestation of solar active region formation and evolution, followed by explosive phenomena(i.e., flares, erupting prominences, coronal mass ejections), and ending with the interaction of plasma magnetized clouds expelled from the Sun with the interplanetary magnetic field and medium. This wide field of research constitutes one of the main aims of COST Action ES0803: Developing Space Weather products and services in Europe. In particular, one of the tasks of this COST Action was to investigate the Progress in Scientific Understanding of Space Weather. In this paper we review the state of the art of our comprehension of some phenomena that, in the scenario outlined above, might have a role on Space Weather, focusing on the researches, thematic reviews, and main results obtained during the COST Action ES0803. Fil: Zuccarello, Francesca. Dipartimento di Astronomia. Universita di Catania; Italia; Fil: Fernando Marcelo López. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Cientifico Tecnológico - Conicet - San Juan. Instituto de Ciencias Astronómicas de la Tierra y del Espacio; Argentina; Fil: Balmaceda, Laura Antonia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Cientifico Tecnológico - CONICET - San Juan. Instituto de Ciencias Astronómicas de la Tierra y del Espacio; Argentina; Fil: Cessateur, Gael. Physical-Meteorological Observatory/World Radiation Center; Suiza; Fil: Cremades, Hebe. Universidad Tecnologica Nacional; Argentina; Fil: Guglielmino, Salvatore. Dipartimento di Astronomia. Universita di Catania; Italia; Fil: Lilensten, Jean. UJF-Grenoble 1/CNRS-INSU. Institut de Plane´tologie et d’Astrophysique de Grenoble; Francia; Fil: Dudok de Wit, Thierry. LPC2E/CNRS (UMR 7328) University of Orleans; Francia; Fil: Kretzschmar, Matthieu. LPC2E/CNRS (UMR 7328) University of Orleans; Francia; Fil: Mierla, Marinela. Solar – Terrestrial Center of Excellence. SIDC. Royal Observatory of Belgium; Bélgica; Fil: Parenti, Susanna. Solar – Terrestrial Center of Excellence. SIDC. Royal Observatory of Belgium; Bélgica; Fil: Pomoell, Jens. Department of Physics. Universidad de Helsinski; Finalndia; Fil: Romano, Paolo. Dipartimento di Astronomia. Universita di Catania; Italia; Fil: Rodriguez, Luciano. Solar – Terrestrial Center of Excellence. SIDC. Royal Observatory of Belgium; Bélgica; Fil: Srivastava, Nandita. Udaipur Solar Observatory. Physical Research laboratory; India; Fil: Vainio, Rami. Department of Physics. Universidad de Helsinski; Finalndia; Fil: West, Matt. Solar – Terrestrial Center of Excellence. SIDC. Royal Observatory of Belgium; Bélgica; Fil: Zuccarello, Francesco P.. Centre for mathematical Plasma Astrophysics; Bélgica
Published: 2013

49. Sun-as-a-Star Observation of Flares in Lyman {\alpha} by the PROBA2/LYRA radiometer

Author: Matthieu Kretzschmar, Ingolf Dammasch, Marie Dominique, Solar-Terrestrial Centre of Excellence [Brussels] (STCE), 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), Belgian Federal Science Policy Office (BELSPO)Swiss Bundesamt fur Bildung und Wissenschaft, European Project: 261948,EC:FP7:SPA,FP7-SPACE-2010-1,ATMOP(2011), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (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 Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: Physics, Radiometer, 010504 meteorology & atmospheric sciences, Solar spectra, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Solar irradiance, 01 natural sciences, law.invention, Wavelength, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, law, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Flare
Abstract: There are very few reports of flare signatures in the solar irradiance at H i Lyman {\alpha} at 121.5 nm, i.e. the strongest line of the solar spectrum. The LYRA radiometer onboard PROBA2 has observed several flares for which unambiguous signatures have been found in its Lyman-{\alpha} channel. Here we present a brief overview of these observations followed by a detailed study of one of them, the M2 flare that occurred on 8 February 2010. For this flare, the flux in the LYRA Lyman-{\alpha} channel increased by 0.6%, which represents about twice the energy radiated in the GOES soft X-ray channel and is comparable with the energy radiated in the He ii line at 30.4 nm. The Lyman-{\alpha} emission represents only a minor part of the total radiated energy of this flare, for which a white-light continuum was detected. Additionally, we found that the Lyman-{\alpha} flare profile follows the gradual phase but peaks before other wavelengths. This M2 flare was very localized and has a very brief impulsive phase, but more statistics are needed to determine if these factors influence the presence of a Lyman-{\alpha} flare signal strong enough to appear in the solar irradiance., Comment: in press for Solar Physics
Published: 2012

50. Solar irradiance observations with PREMOS filter radiometers on the PICARD mission: In-flight performance and data release

Author: Julian Gröbner, S. Nyeki, Peter Meindl, T. Egorova, Wolfgang Finsterle, Gaël Cessateur, Jean-François Hochedez, Rinat Tagirov, Mustapha Meftah, G. Thuillier, Christoph Wehrli, M. Rouzé, Hansjörg Roth, Alexander Shapiro, Werner Schmutz, Eugene Rozanov, Nigel Fox, Matthieu Kretzschmar, S. Koller, Micha Schöll, M. Haberreiter, Marcel Spescha, Daniel Pfiffner, Lutz Werner, Jules U Wyss, Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), Institute for Atmospheric and Climate Science [Zürich] (IAC), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, STRATO - 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), National Physical Laboratory [Teddington] (NPL), Physikalisch-Technische Bundesanstalt [Berlin] (PTB), Centre National d'Études Spatiales [Toulouse] (CNES), European Community’s Seventh Framework Programme (FP7/2007-2013), CNES/PICARD GI programme, European Project: 313188,EC:FP7:SPA,FP7-SPACE-2012-1,SOLID(2012), European Project: 284461,EC:FP7:SPA,FP7-SPACE-2011-1,EHEROES(2012), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), and Max-Planck-Institut für Sonnensystemforschung (MPS)
Subjects: 010504 meteorology & atmospheric sciences, Meteorology, Infrared, Solar activity, Irradiance, Venus, Radiation, Solar irradiance, 01 natural sciences, 7. Clean energy, Instrumentation: photometers, UV radiation, 0103 physical sciences, Solar radiation, Solstice, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, Physics, Radiometer, biology, Spacecraft, business.industry, Astronomy and Astrophysics, biology.organism_classification, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 13. Climate action, Space and Planetary Science, Solar-terrestrial relations, business
Abstract: International audience; The PREcision Monitoring Sensor (PREMOS) is a solar radiometer on board the French PICARD mission that was launched in June 2010 and decommissioned in April 2014.Aims. The PREMOS radiometer obtains solar irradiance measurements in specific spectral windows in the UV, visible, and near- infrared. In this paper, the PREMOS data and calibration methods are presented.Methods. Using back-up channels, the degradation can theoretically be assessed to correct operational channels. However, a strong degradation within all PREMOS channels requires the application of additional methods, namely using back-up channels and assess- ing the degradation via a proxy-based model.Results. The corrected Level 3 PREMOS data are then used in different contexts in order to be validated. First, the signature of the p-mode are retrieved from the PREMOS data. The Venus transit allows us to empirically determine the intrinsic noise level within the PREMOS high cadence data for the visible and near-infrared channels. We then compare the PREMOS data directly to other data sets, namely from the SOLar-STellar Irradiance Comparison Experiment (SOLSTICE) and the Solar Irradiance Monitor (SIM) instru- ments on board the SOlar Radiation and Climate Experiment (SORCE) spacecraft. Regarding the UV channels, we found an excellent correlation over the lifetime of the PREMOS mission. The ratio between SORCE and PREMOS observations is always less than 1%. Regarding the SSI measurements in the visible and near-infrared, a comparison of short-term variations (i.e. 27-day modulation) shows a rather good correlation by taking into consideration the intrinsic noise within both SIM and PREMOS observations.
Published: 2016

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