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11 results on '"H. Önel"'

1. 4MOST: the 4-metre Multi-Object Spectroscopic Telescope project status: instrument manufacturing and integration, operations development, and survey planning

Author

Samual C. Barden, Norbert Christlieb, Else Starkenburg, Jean-Paul Kneib, Wolfgang Gaessler, Thomas Bensby, Jörg Knoche, Johan Pragt, Johan Comparat, H. Önel, Man I. Lam, Johan Richard, Andreas Kelz, J. Walcher, Florian Rothmaier, Maria Bergemann, Roland Winkler, Isabella Cesarini, Amina Helmi, Clare Worley, Mike Irwin, Ingo Stilz, Mark Sullivan, Andrea Merloni, Domenico Giannone, Steffen Frey, Diana Johl, Jean-Francois Pirard, Maria-Rosa L. Cioni, Matthias Steinmetz, Genoveva Micheva, Simon P. Driver, Alban Remilleux, Vincenzo Mainieri, Joar Brynnel, Nicholas A. Walton, Roelof S. de Jong, Cristina Chiappini, Richard G. McMahon, Sofia Feltzing, Ivan Minchev, Scott Smedley, Olga Bellido-Tirado, and Jochen Liske

Subjects
Large field of view, Computer science, business.industry, Object (computer science), Wide field, law.invention, Telescope, law, Systems engineering, Metre, System integration, Community survey, business, Spectrograph
Abstract

A status overview of 4MOST is presented, a new high-multiplex, wide-field spectroscopic survey facility under construction for ESO's VISTA telescope at Paranal. Its key specifications are: a large field of view of 4.4 deg2 and a high multiplex capability, with 1624 fibres feeding two low-resolution spectrographs (R = λ/Δλ ~ 6500), and 812 fibres transferring light to the high-resolution spectrograph (R ~ 20 000). The 4MOST system integration has commenced and the selection process for ESO community survey programmes has been started. This overview presents the expected performance of the instrument, the science the consortium expects to carry out, and the unique operational scheme of 4MOST.

Published
2020

2. The Energetic Particle Detector. Energetic particle instrument suite for the Solar Orbiter mission

Author

Milan Maksimovic, G. M. Mason, M. E. Wiedenbeck, S. Kolbe, Pertti Makela, A. Ravanbakhsh, N. Vilmer, C. Gordillo, L. Seimetz, Lauri Panitzsch, A. da Silva Fariña, A. Russu, R. Elftmann, Stephan Böttcher, J. R. Hayes, R. Paspirgilis, Aarón Montalvo, S. Begley, Säm Krucker, Óscar Ramón Ramos Gutiérrez, Pablo Parra, Alberto Carrasco, Eduard P. Kontar, Andrew Walsh, Sebastián Sánchez-Prieto, Stefan J. Hofmeister, Karl-Ludwig Klein, J. Tammen, E. Böhm, Olga Malandraki, B. Schuster, K. S. Nelson, F. Espinosa Lara, Jia Yu, Manuel Prieto, Arik Posner, W. Dröge, Neus Agueda, O. Gevin, I. Sánchez, Raúl Gómez-Herrero, C. Terasa, K. Tyagi, Rami Vainio, A. R. Dupont, Juan Jose Blanco, C. E. Schlemm, Angels Aran, Q. Zong, James M. Ryan, A. Kulemzin, Matthew E. Hill, David Lario, Jan Soucek, Jan Köhler, Cesar Martin, Karel Kudela, Robert F. Wimmer-Schweingruber, G. C. Ho, S. Kerem, Javier Rodriguez-Pacheco, T. I. Varela, O. Rodríguez-Polo, D. Meziat, Bernd Heber, O. Limousin, K. Wirth, V. Knierim, D. Pacheco, V. de Manuel González, H. Seifert, J. Almena, Christopher J. Owen, Yulia Kartavykh, Shrinivasrao R. Kulkarni, S. Boden, A. Martínez Hellín, J. J. Connell, S. Eldrum, Christian Drews, H. Önel, I. Cernuda, R. Castillo, Natchimuthuk Gopalswamy, S. Liang, W. J. Lees, Dennis Haggerty, M. Jüngling, Linghua Wang, W. Boogaerts, Silvia Dalla, B. Klecker, Timothy S. Horbury, M. Yedla, M. L Richards, G. B. Andrews, Jan Steinhagen, Blai Sanahuja, G. Mann, Universidad de Alcalá - University of Alcalá (UAH), Institut für Experimentelle und Angewandte Physik [Kiel] (IEAP), Christian-Albrechts-Universität zu Kiel (CAU), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Universidad de Tarapaca, Paul Scherrer Institute (PSI), Indian Institute of Technology Bombay (IIT Bombay), 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), and Science and Technology Facilities Council (STFC)

Subjects
Sun: flares, 010504 meteorology & atmospheric sciences, Sun: coronal mass ejections (CMEs), Population, Astrophysics, Astronomy & Astrophysics, FOCUSED TRANSPORT, 01 natural sciences, Particle detector, Particle identification, law.invention, Orbiter, law, Sun: particle emission, 0201 Astronomical and Space Sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Sun: heliosphere, education, 010303 astronomy & astrophysics, acceleration of particles, HIGH-ENERGIES, 0105 earth and related environmental sciences, Physics, education.field_of_study, Science & Technology, INTERPLANETARY SHOCKS, Solar energetic particles, instrumentation: detectors, Ecliptic, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, COSMIC-RAYS, ADIABATIC DECELERATION, CORONAL MASS EJECTIONS, SPACECRAFT OBSERVATIONS, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physical Sciences, Physics::Space Physics, SEP EVENTS, Heliospheric current sheet, Astrophysics::Earth and Planetary Astrophysics, PROTON PEAK INTENSITIES, MONTE-CARLO SIMULATIONS, Heliosphere
Abstract

International audience; After decades of observations of solar energetic particles from space-based observatories, relevant questions on particle injection, transport, and acceleration remain open. To address these scientific topics, accurate measurements of the particle properties in the inner heliosphere are needed. In this paper we describe the Energetic Particle Detector (EPD), an instrument suite that is part of the scientific payload aboard the Solar Orbiter mission. Solar Orbiter will approach the Sun as close as 0.28 au and will provide extra-ecliptic measurements beyond ∼30° heliographic latitude during the later stages of the mission. The EPD will measure electrons, protons, and heavy ions with high temporal resolution over a wide energy range, from suprathermal energies up to several hundreds of megaelectronvolts/nucleons. For this purpose, EPD is composed of four units: the SupraThermal Electrons and Protons (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) plus the Instrument Control Unit that serves as power and data interface with the spacecraft. The low-energy population of electrons and ions will be covered by STEP and EPT, while the high-energy range will be measured by HET. Elemental and isotopic ion composition measurements will be performed by SIS and HET, allowing full particle identification from a few kiloelectronvolts up to several hundreds of megaelectronvolts/nucleons. Angular information will be provided by the separate look directions from different sensor heads, on the ecliptic plane along the Parker spiral magnetic field both forward and backwards, and out of the ecliptic plane observing both northern and southern hemispheres. The unparalleled observations of EPD will provide key insights into long-open and crucial questions about the processes that govern energetic particles in the inner heliosphere.

Published
2020

3. The Spectrometer/Telescope for Imaging X-rays (STIX)

Author

Robert P. Lin, N. Vilmer, G. J. Hurford, S. Kobler, H. J. Wiehl, Konrad Rutkowski, M. Winkler, Brian R. Dennis, F. Marone, Diego Casadei, M. Michalska, I. Le Mer, L. Etesi, Jana Kašparová, Michele Piana, O. Gevin, D. Schori, G. Juchnikowski, Frank Dionies, G. Birrer, J. Anderson, H.-P. Gröbelbauer, H. Xiao, M. Darmetko, Karol Seweryn, Milan Maksimovic, Marek Siarkowski, Oliver Grimm, Säm Krucker, Ewan C. Dickson, S. Felix, K. Lapadula, Anna Maria Massone, Antoine Strugarek, H. F. van Beek, Federico Benvenuto, O. Limousin, Marek Stęślicki, R. A. Schwartz, N. Hochmuth, S. Kögl, Tomasz Mrozek, N. G. Arnold, Konrad Skup, Waldemar Bujwan, M. Kuhar, M. Woche, L. Iseli, G. Mann, D. Ścisłowski, F. Molendini, Martin Bednarzik, Erica Lastufka, St. Stutz, F. Schuller, Piotr Orleanski, S. Brun, Ch. Wild, Andrzej Cichocki, Alexander Warmuth, Paolo Massa, K. Ber, Janusz Sylwester, A. Białek, Arnold O. Benz, Peter T. Gallagher, Sophie Musset, M. Dreier, H. Önel, H. Sathiapal, Lucia Kleint, Piotr Podgorski, Z. Kozáček, D. S. Bloomfield, J. Paschke, F. Schramka, D. Plüschke, Javier Rodriguez-Pacheco, Piotr Osica, J. Rendtel, André Csillaghy, Svend-Marian Bauer, Shane A. Maloney, Simon Marcin, Astrid M. Veronig, Marina Battaglia, František Fárník, A. Meuris, Miroslaw Kowalinski, 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 d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Imaging spectrometer, F500, Astrophysics, 7. Clean energy, 01 natural sciences, law.invention, Telescope, Orbiter, Optics, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Spectrometer, Solar flare, Sun: corona, business.industry, Sun: chromosphere, Gamma ray, Bremsstrahlung, instrumentation: miscellaneous, Sun: X-rays, gamma rays, Sun: chromosphere, Sun: corona, Astronomy and Astrophysics, instrumentation: miscellaneous, gamma rays, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Sun: X-rays, Flare
Abstract

Aims. The Spectrometer Telescope for Imaging X-rays (STIX) on Solar Orbiter is a hard X-ray imaging spectrometer, which covers the energy range from 4 to 150 keV. STIX observes hard X-ray bremsstrahlung emissions from solar flares and therefore provides diagnostics of the hottest (⪆10 MK) flare plasma while quantifying the location, spectrum, and energy content of flare-accelerated nonthermal electrons. Methods. To accomplish this, STIX applies an indirect bigrid Fourier imaging technique using a set of tungsten grids (at pitches from 0.038 to 1 mm) in front of 32 coarsely pixelated CdTe detectors to provide information on angular scales from 7 to 180 arcsec with 1 keV energy resolution (at 6 keV). The imaging concept of STIX has intrinsically low telemetry and it is therefore well-suited to the limited resources available to the Solar Orbiter payload. To further reduce the downlinked data volume, STIX data are binned on board into 32 selectable energy bins and dynamically-adjusted time bins with a typical duration of 1 s during flares. Results. Through hard X-ray diagnostics, STIX provides critical information for understanding the acceleration of electrons at the Sun and their transport into interplanetary space and for determining the magnetic connection of Solar Orbiter back to the Sun. In this way, STIX serves to link Solar Orbiter’s remote and in-situ measurements.

Published
2020

4. Models and data analysis tools for the Solar Orbiter mission

Author

Kamen Kozarev, Hardi Peter, X. Bonnin, Manolis K. Georgoulis, Alexis P. Rouillard, Daniele Spadaro, A. De Groof, Angels Aran, Raul Gomez-Herrero, M. Bouchemit, Alessandro Bemporad, R. A. Howard, A. S. Brun, F. Espinosa Lara, E. Budnik, S. I. Jones, N. E. Raouafi, Rita Ventura, J. C. del Toro Iniesta, David Pérez-Suárez, Silvano Fineschi, Miho Janvier, Jon A. Linker, Thomas Wiegelmann, Teresa Nieves-Chinchilla, Timothy S. Horbury, L. R. Bellot Rubio, A. Giunta, Nicolas Poirier, Bogdan Nicula, Andreas Lagg, Kévin Dalmasse, Jim M. Raines, Michael Lavarra, Carl J. Henney, Holly Gilbert, S. Parenti, D. Orozco Suárez, Mikel Indurain, David R. Williams, David Berghmans, L. Etesi, Andrzej Fludra, F. Auchère, Daniel Müller, Vincent Génot, Y. Wu, Jens Pomoell, Marco Romoli, N. Rich, A. Kouloumvakos, S. Caminade, Benoit Lavraud, Antoine Strugarek, G. Mann, Philippe Louarn, Arnaud Masson, J. Carlyle, L. Sanchez, I. Zouganelis, Baptiste Cecconi, Eric Buchlin, Javier Rodriguez-Pacheco, T. Amari, M. Haberreiter, Thomas Straus, C. Watson, Alexander Warmuth, Johann Hirzberger, Säm Krucker, Athanasios Papaioannou, Tino L. Riethmüller, Pedro Osuna, Cis Verbeeck, Shane A. Maloney, William T. Thompson, Luciano Rodriguez, Sami K. Solanki, H. Önel, Paolo Pagano, I. Cernuda, Andrei Fedorov, Luca Teriaca, E. Kraaikamp, Nicole Vilmer, Rui F. Pinto, S. Dolei, Simon Plunkett, Roberto Susino, Etienne Pariat, Andrew Walsh, Clementina Sasso, Vincenzo Andretta, Christopher J. Owen, Donald M. Hassler, S. Guest, O. C. St. Cyr, Anastasios Anastasiadis, Ester Antonucci, Angelos Vourlidas, Andrei Zhukov, Milan Maksimovic, C. N. Arge, Matthieu Alexandre, Joseph M. Davila, Centre de Physique Théorique [Palaiseau] (CPHT), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Space Physics Research Group, 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), Naval Research Laboratory (NRL), European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astrofisico di Catania (OACT), 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), National Center for Atmospheric Research [Boulder] (NCAR), Laboratoire de Physique des Plasmas (LPP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Institut de Recherche sur la Fusion par confinement Magnétique (IRFM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Stéréochimie et Interactions Moléculaires (STIM), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Royal Observatory of Belgium [Brussels] (ROB), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Centre de Recherche en Transplantation et Immunologie (U1064 Inserm - CRTI), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Nantes - UFR de Médecine et des Techniques Médicales (UFR MEDECINE), Université de Nantes (UN)-Université de Nantes (UN), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), INAF - Osservatorio Astronomico di Capodimonte (OAC), Institut Jacques Monod (IJM (UMR_7592)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Solar-Terrestrial Centre of Excellence [Brussels] (STCE), 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), NOVELTIS [Sté], Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], NASA Goddard Space Flight Center (GSFC), 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Blackett Laboratory, Imperial College London, EADS Astrium SAS, Science Applications International Corporation (SAIC), Space Science and Applications, Los Alamos National Laboratory (LANL), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Trinity College Dublin, Leibniz-Institut für Astrophysik Potsdam (AIP), Laboratoire Francis PERRIN (LFP - URA 2453), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut d'Electronique du Solide et des Systèmes (InESS), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centro de Investigacion Cientifica y de Education Superior de Ensenada [Mexico] (CICESE), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Ecosystèmes et paysages montagnards (UR EPGR), Centre national du machinisme agricole, du génie rural, des eaux et forêts (CEMAGREF), Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (INFN, Sezione di Napoli), Istituto Nazionale di Fisica Nucleare (INFN), Max Planck Institute for Solar System Research (MPS), 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 Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Microbiology Department, St. Jame's Hospital, European Research Council, European Commission, Science and Technology Facilities Council (UK), Durham University, Centre National D'Etudes Spatiales (France), Helmholtz Association, German Centre for Air and Space Travel, Ministerio de Ciencia, Innovación y Universidades (España), 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), 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), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), 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), ANR-17-CE31-0006,COROSHOCK,EVALUER LE ROLE DU CHOC COMME ACCELERATEUR DE PARTICULES SOLAIRES(2017), 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 d'Orléans (UO), Rouillard A.P., Pinto R.F., Vourlidas A., De Groof A., Thompson W.T., Bemporad A., Dolei S., Indurain M., Buchlin E., Sasso C., Spadaro D., Dalmasse K., Hirzberger J., Zouganelis I., Strugarek A., Brun A.S., Alexandre M., Berghmans D., Raouafi N.E., Wiegelmann T., Pagano P., Arge C.N., Nieves-Chinchilla T., Lavarra M., Poirier N., Amari T., Aran A., Andretta V., Antonucci E., Anastasiadis A., Auchere F., Bellot Rubio L., Nicula B., Bonnin X., Bouchemit M., Budnik E., Caminade S., Cecconi B., Carlyle J., Cernuda I., Davila J.M., Etesi L., Espinosa Lara F., Fedorov A., Fineschi S., Fludra A., Genot V., Georgoulis M.K., Gilbert H.R., Giunta A., Gomez-Herrero R., Guest S., Haberreiter M., Hassler D., Henney C.J., Howard R.A., Horbury T.S., Janvier M., Jones S.I., Kozarev K., Kraaikamp E., Kouloumvakos A., Krucker S., Lagg A., Linker J., Lavraud B., Louarn P., Maksimovic M., Maloney S., Mann G., Masson A., Muller D., Onel H., Osuna P., Orozco Suarez D., Owen C.J., Papaioannou A., Perez-Suarez D., Rodriguez-Pacheco J., Parenti S., Pariat E., Peter H., Plunkett S., Pomoell J., Raines J.M., Riethmuller T.L., Rich N., Rodriguez L., Romoli M., Sanchez L., Solanki S.K., St Cyr O.C., Straus T., Susino R., Teriaca L., Del Toro Iniesta J.C., Ventura R., Verbeeck C., Vilmer N., Warmuth A., Walsh A.P., Watson C., Williams D., Wu Y., Zhukov A.N., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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), vilmer, nicole, and University of St Andrews. Applied Mathematics

Subjects
010504 meteorology & atmospheric sciences, corona [Sun], Solar wind, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 7. Clean energy, 01 natural sciences, law.invention, Data acquisition, law, Coronal mass ejection, general [Sun], QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Sun: magnetic fields, QC, ComputingMilieux_MISCELLANEOUS, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 3rd-DAS, energetic particles, CORONAL MASS EJECTIONS, numerical modeling, magnetic fields [Sun], solar wind, Physics::Space Physics, Systems engineering, Astrophysics::Earth and Planetary Astrophysics, atmosphere [Sun], fundamental parameters [Sun], Sun: general, FORCE-FREE FIELD, Sun: fundamental parameters, Solar radius, Context (language use), STREAMER STRUCTURE, Orbiter, 0103 physical sciences, OPTIMIZATION APPROACH, [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], POLARIZATION MEASUREMENTS, Sun: Solar wind, 3-DIMENSIONAL STRUCTURE, 0105 earth and related environmental sciences, Spacecraft, business.industry, Sun: corona, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], solar corona, MAGNETIC-FLUX ROPES, Astronomy and Astrophysics, SHOCKS DRIVEN, 115 Astronomy, Space science, SPECTRAL-LINES, QC Physics, 13. Climate action, Space and Planetary Science, business, Heliosphere, Sun: atmosphere, ELECTRON-DENSITY
Abstract

All authors: Rouillard, A. P.; Pinto, R. F.; Vourlidas, A.; De Groof, A.; Thompson, W. T.; Bemporad, A.; Dolei, S.; Indurain, M.; Buchlin, E.; Sasso, C.; Spadaro, D.; Dalmasse, K.; Hirzberger, J.; Zouganelis, I.; Strugarek, A.; Brun, A. S.; Alexandre, M.; Berghmans, D.; Raouafi, N. E.; Wiegelmann, T.; Pagano, P.; Arge, C. N.; Nieves-Chinchilla, T.; Lavarra, M.; Poirier, N.; Amari, T.; Aran, A.; Andretta, V.; Antonucci, E.; Anastasiadis, A.; Auchère, F.; Bellot Rubio, L.; Nicula, B.; Bonnin, X.; Bouchemit, M.; Budnik, E.; Caminade, S.; Cecconi, B.; Carlyle, J.; Cernuda, I.; Davila, J. M.; Etesi, L.; Espinosa Lara, F.; Fedorov, A.; Fineschi, S.; Fludra, A.; Génot, V.; Georgoulis, M. K.; Gilbert, H. R.; Giunta, A.; Gomez-Herrero, R.; Guest, S.; Haberreiter, M.; Hassler, D.; Henney, C. J.; Howard, R. A.; Horbury, T. S.; Janvier, M.; Jones, S. I.; Kozarev, K.; Kraaikamp, E.; Kouloumvakos, A.; Krucker, S.; Lagg, A.; Linker, J.; Lavraud, B.; Louarn, P.; Maksimovic, M.; Maloney, S.; Mann, G.; Masson, A.; Müller, D.; Önel, H.; Osuna, P.; Orozco Suarez, D.; Owen, C. J.; Papaioannou, A.; Pérez-Suárez, D.; Rodriguez-Pacheco, J.; Parenti, S.; Pariat, E.; Peter, H.; Plunkett, S.; Pomoell, J.; Raines, J. M.; Riethmüller, T. L.; Rich, N.; Rodriguez, L.; Romoli, M.; Sanchez, L.; Solanki, S. K.; St Cyr, O. C.; Straus, T.; Susino, R.; Teriaca, L.; del Toro Iniesta, J. C.; Ventura, R.; Verbeeck, C.; Vilmer, N.; Warmuth, A.; Walsh, A. P.; Watson, C.; Williams, D.; Wu, Y.; Zhukov, A. N.-- Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. The Solar Orbiter spacecraft will be equipped with a wide range of remote-sensing (RS) and in situ (IS) instruments to record novel and unprecedented measurements of the solar atmosphere and the inner heliosphere. To take full advantage of these new datasets, tools and techniques must be developed to ease multi-instrument and multi-spacecraft studies. In particular the currently inaccessible low solar corona below two solar radii can only be observed remotely. Furthermore techniques must be used to retrieve coronal plasma properties in time and in three dimensional (3D) space. Solar Orbiter will run complex observation campaigns that provide interesting opportunities to maximise the likelihood of linking IS data to their source region near the Sun. Several RS instruments can be directed to specific targets situated on the solar disk just days before data acquisition. To compare IS and RS, data we must improve our understanding of how heliospheric probes magnetically connect to the solar disk. Aims. The aim of the present paper is to briefly review how the current modelling of the Sun and its atmosphere can support Solar Orbiter science. We describe the results of a community-led effort by European Space Agency's Modelling and Data Analysis Working Group (MADAWG) to develop different models, tools, and techniques deemed necessary to test different theories for the physical processes that may occur in the solar plasma. The focus here is on the large scales and little is described with regards to kinetic processes. To exploit future IS and RS data fully, many techniques have been adapted to model the evolving 3D solar magneto-plasma from the solar interior to the solar wind. A particular focus in the paper is placed on techniques that can estimate how Solar Orbiter will connect magnetically through the complex coronal magnetic fields to various photospheric and coronal features in support of spacecraft operations and future scientific studies. Methods. Recent missions such as STEREO, provided great opportunities for RS, IS, and multi-spacecraft studies. We summarise the achievements and highlight the challenges faced during these investigations, many of which motivated the Solar Orbiter mission. We present the new tools and techniques developed by the MADAWG to support the science operations and the analysis of the data from the many instruments on Solar Orbiter. Results. This article reviews current modelling and tool developments that ease the comparison of model results with RS and IS data made available by current and upcoming missions. It also describes the modelling strategy to support the science operations and subsequent exploitation of Solar Orbiter data in order to maximise the scientific output of the mission. Conclusions. The on-going community effort presented in this paper has provided new models and tools necessary to support mission operations as well as the science exploitation of the Solar Orbiter data. The tools and techniques will no doubt evolve significantly as we refine our procedure and methodology during the first year of operations of this highly promising mission. © 2020 A. P. Rouillard et al., Solar Orbiter is a joint ESA and NASA mission. A. Vourlidas' Solar Orbiter effort is supported by NRL grant N00173-16-1-G029. P. Pagano would like to thank D. H. Mackay and S. L. Yardley for their valuable contributions, the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 647214), and the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (http://www.dirac.ac.uk).This equipment was funded by a BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/K00087X/1, DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. A. Rouillard, V. Genot, M. Janvier, Elie Soubrier, F. Auchere, E. Buchlin and E. Pariat acknowledge support from the French space agency (Centre National d'Etudes Spatiales; CNES; https://cnes.fr/fr) that funds activity in plasma physics data center (Centre de Donnees de la Physique des Plasmas; CDPP; http://cdpp.eu/) and the Multi Experiment Data and Operation Center (MEDOC; https://idoc.ias.u-psud.fr/MEDOC), and the space weather team in Toulouse (Solar-Terrestrial Observations and Modelling Service; STORMS; http://storms-service.irap.omp.eu/).This includes funding for Gaia-DEM, the data mining tools AMDA (http://amda.cdpp.eu/), CLWEB (clweb.cesr. fr/) and the propagation tool (http://propagationtool.cdpp.eu).R.Pinto, M. Lavarra, Y. Wu and A. Kouloumvakos acknowledge financial support from the ANR project SLOW_ SOURCE No. ANR-17-CE31-0006-01, ANR project COROSHOCK No. ANR-18-ERC1-0006-01 and FP7 HELCATS project https://www.helcats-fp7.eu/under the FP7 EU contract number 606692. A. Warmuth acknowledges the support by DLR under grant No. 50 QL 0001. The STEREO SECCHI data are produced by a consortium of RAL (UK), NRL (USA), LMSAL (USA), GSFC (USA), MPS (Germany), CSL (Belgium), IOTA (France) and IAS (France). The ACE data were obtained from the ACE science center. The WIND data were obtained from the Space Physics Data Facility. Javier Rodriguez-Pacheco acknowledges Spanish Project: FEDER/MCIU-AEI/Project ESP2017-88436-R.

Published
2020

5. The STIX Aspect System (SAS): The Optical Aspect System of the Spectrometer/Telescope for Imaging X-Rays (STIX) on Solar Orbiter

Author

H.-P. Gröbelbauer, W. Bittner, Svend-Marian Bauer, C. Denker, Frank Dionies, Waldemar Bujwan, Piotr Orleanski, D. Plüschke, Alexander Warmuth, Klaus G. Strassmeier, J. Paschke, H. J. Wiehl, J. Anderson, G. Mann, K. Ber, G. J. Hurford, F. Schuller, H. Önel, D. P. Sablowski, V. Senthamizh Pavai, André Csillaghy, N. G. Arnold, Konrad Rutkowski, Diego Casadei, S. Kögl, Konrad Skup, Säm Krucker, Jürgen Rendtel, Oliver Grimm, D. Schori, and M. Woche

Subjects
Physics, Solar flare, Spectrometer, Spacecraft, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Bremsstrahlung, Astronomy and Astrophysics, 01 natural sciences, Corona, Photodiode, law.invention, 010309 optics, Telescope, Orbiter, Optics, Space and Planetary Science, law, Physics::Space Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, 010303 astronomy & astrophysics
Abstract

The Spectrometer/Telescope for Imaging X-rays (STIX) is a remote sensing instrument on Solar Orbiter that observes the hard X-ray bremsstrahlung emission of solar flares. This paper describes the STIX Aspect System (SAS), a subunit that measures the pointing of STIX relative to the Sun with a precision of $\pm 4''$ , which is required to accurately localize the reconstructed X-ray images on the Sun. The operating principle of the SAS is based on an optical lens that images the Sun onto a plate that is perforated by small apertures arranged in a cross-shaped configuration of four radial arms. The light passing through the apertures of each arm is detected by a photodiode. Variations of spacecraft pointing and of distance from the Sun cause the solar image to move over different apertures, leading to a modulation of the measured lightcurves. These signals are used by ground analysis to calculate the locations of the solar limb, and hence the pointing of the telescope.

Published
2020

6. Connecting the Properties of Coronal Shock Waves with Those of Solar Energetic Particles

Author

Athanasios Kouloumvakos, Alexis P. Rouillard, Rami Vainio, Illya Plotnikov, Alexandr Afanasiev, H. Önel, Yihong Wu, Angelos Vourlidas, 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), National Laboratory of Pattern Recognition [Beijing] (NLPR), Institute of Automation - Chinese Academy of Sciences, Department of Engineering Physics, Helsinki University of Technology, PO Box 4100, FI-02015 HUT, FINLAND, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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 ANR-17-CE31-0006,COROSHOCK,EVALUER LE ROLE DU CHOC COMME ACCELERATEUR DE PARTICULES SOLAIRES(2017)

Subjects
Shock wave, Physics, Range (particle radiation), 010504 meteorology & atmospheric sciences, Spacecraft, Solar energetic particles, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Solar cycle 24, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Computational physics, Shock (mechanics), Particle acceleration, symbols.namesake, Mach number, Space and Planetary Science, 0103 physical sciences, Physics::Space Physics, symbols, Astrophysics::Solar and Stellar Astrophysics, business, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract

International audience; We develop and exploit a new catalog of coronal pressure waves modeled in 3D to study the potential role of these waves in accelerating solar energetic particles (SEPs) measured in situ. Our sample comprises modeled shocks and SEP events detected during solar cycle 24 observed over a broad range of longitudes. From the 3D reconstruction of shock waves using coronagraphic observations we derived the 3D velocity along the entire front as a function of time. Combining new reconstruction techniques with global models of the solar corona, we derive the 3D distribution of basic shock parameters such as Mach numbers, compression ratios, and shock geometry. We then model in a time-dependent manner how the shock wave connects magnetically with spacecraft making in situ measurements of SEPs. This allows us to compare modeled shock parameters deduced at the magnetically well-connected regions, with different key parameters of SEPs such as their maximum intensity. This approach accounts for projection effects associated with remote-sensing observations and constitutes the most extensive study to date of shock waves in the corona and their relation to SEPs. We find a high correlation between the maximum flux of SEPs and the strength of coronal shock waves quantified, for instance, by the Mach number. We discuss the implications of that work for understanding particle acceleration in the corona.

Published
2019

7. Propagation of energetic electrons through the solar corona and the interplanetary medium

Author

G. Mann, H. Önel, and Erwin Sedlmayr

Subjects
Physics, Solar flare, Space and Planetary Science, Electric field, Coulomb, Interplanetary medium, Astronomy and Astrophysics, Electron, Astrophysics, Pitch angle, Plasma, Magnetic field
Abstract

Aims. The electron transport is investigated numerically after an electron transport model is deduced. Methods. This model for electron propagation considers global electric and magnetic fields, as well as local Coulomb collisions. A new way to handle the electron's pitch angle evolution by using a binary dice within the treatment of the Coulomb scattering is introduced. The conditions in the solar plasma are represented by average and commonly used models, such that numerical simulations can be performed easily. Results. The model for electron propagation finally obtained makes it possible to investigate how the Coulomb collisions act on the pitch angle, while electrons are transported through the solar plasma. Some chosen numerical results for different initial conditions are presented in the paper.

Published
2006

8. The spectrometer/telescope for imaging X-rays on board the ESA Solar Orbiter spacecraft

Author

Oliver Grimm, N. Vilmer, J. Rendtel, V. Commichau, W. Bittner, Frank Dionies, H. J. Wiehl, Gottfried Mann, Marcin Stolarski, D. Plüschke, Säm Krucker, H. F. van Beek, Arnold O. Benz, Piotr Podgorski, Olivier Limousin, G. Viertel, N. Hochmuth, Emil Popow, Janusz Sylwester, A. Białek, Robert P. Lin, M. Mosdorf, S. Kobler, Svend-Marian Bauer, A. Meuris, Martin Bednarzik, Konrad Skup, Piotr Orleanski, D. Wolter, H. Önel, J. Paschke, L. Iseli, Alexander Warmuth, S. Brun, N. G. Arnold, H.-P. Gröbelbauer, W. Nowosielski, M. Woche, L. Etesi, André Csillaghy, Rafal Graczyk, M. Michalska, G. J. Hurford, Karol Seweryn, Tomasz Mrozek, Henry Aurass, D. Casadei, R. Resanovic, Andrzej Cichocki, Marina Battaglia, Miroslaw Kowalinski, František Fárník, Andrew W. Howard, European Organization for Nuclear Research (CERN), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), University of Leeds, Institute of Atmospheric Physics [Prague] (IAP), and Czech Academy of Sciences [Prague] (CAS)

Subjects
Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, Imaging spectrometer, 7. Clean energy, 01 natural sciences, 030218 nuclear medicine & medical imaging, law.invention, Telescope, 03 medical and health sciences, Orbiter, 0302 clinical medicine, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Instrumentation, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Spectrometer, Solar flare, Spacecraft, 010308 nuclear & particles physics, business.industry, Bremsstrahlung, Astronomy, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Heliosphere
Abstract

Solar Orbiter is a Sun-observing mission led by the European Space Agency, addressing the interaction between the Sun and the heliosphere. It will carry ten instruments, among them the X-ray imaging spectrometer STIX. STIX will determine the intensity, spectrum, timing, and location of thermal and accelerated electrons near the Sun through their bremsstrahlung X-ray emission. This report gives a brief overview of the STIX scientific goals and covers in more detail the instrument design and challenges.

Published
2013

9. Instrument data processing unit for spectrometer/telescope for imaging x-rays (STIX)

Author

Michał Mosdorf, Witold Nowosielski, Karol Seweryn, Miroslaw Kowalinski, Oliver Grimm, N. G. Arnold, Rafal Graczyk, Piotr Podgorski, M. Michalska, O. Limousin, G. J. Hurford, A. Przepiórka, H. Önel, Andrzej Cichocki, Säm Krucker, Marek Winkler, Piotr Orleanski, Konrad Skup, Janusz Sylwester, Marcin Stolarski, A. Meuris, Arnold O. Benz, and Tomasz Mrozek

Subjects
Physics, Data processing, Spectrometer, business.industry, Instrument Data, law.invention, Data processing system, Telescope, Imaging spectroscopy, Orbiter, Software, Optics, law, business, Remote sensing
Abstract

The Spectrometer/Telescope for Imaging X-rays (STIX) is one of 10 instruments on board Solar Orbiter, an M-class mission of the European Space Agency (ESA) scheduled to be launch in 2017. STIX applies a Fourier-imaging technique using a set of tungsten grids in front of 32 pixelized CdTe detectors to provide imaging spectroscopy of solar thermal and non-thermal hard X-ray emissions from 4 to 150 keV. These detectors are source of data collected and analyzed in real-time by Instrument Data Processing Unit (IDPU). Besides the data processing the IDPU controls and manages other STIX’s subsystems: ASICs and ADCs associated with detectors, Aspect System, Attenuator, PSU and HK. The instrument reviewed in this paper is based on the design that passed the Instrument Preliminary Design Review (IPDR) in early 2012 and Software Preliminary Design Review (SW PDR) in middle of 2012. Particular emphasis is given to the IDPU and low level software called Basic SW (BSW).

Published
2012

10. The spectrometer telescope for imaging x-rays on board the Solar Orbiter mission

Author

Michał Mosdorf, Henry Aurass, Piotr Orleanski, André Csillaghy, Gottfried Mann, Anna Maria Massone, Emil Popow, Piotr Podgorski, Svend-Marian Bauer, A. Meuris, L. Iseli, I. W. Kienreich, G. J. Hurford, Jana Kašparová, Brian R. Dennis, H.-P. Gröbelbauer, Karol Seweryn, N. Vilmer, H. J. Wiehl, Olivier Limousin, G. Viertel, M. Piana, Janusz Sylwester, Martin Bednarzik, Alexander Warmuth, S. Klober, N. Hochmuth, František Fárník, J. Paschke, Peter T. Gallagher, Oliver Grimm, Rafal Graczyk, Säm Krucker, V. Commichau, Marcin Stolarski, Arnold O. Benz, M. Michalska, Frank Dionies, Konrad Skup, D. Wolker, R. A. Schwarz, Marina Battaglia, D. Plüschke, A. Przepiórka, W. Bittner, J. Rendtel, M. Woche, H. F. van Beek, Miroslaw Kowalinski, Tomasz Mrozek, L. Etesi, Astrid Veronig, Witold Nowosielski, S. Brun, Robert P. Lin, N. G. Arnold, D. S. Bloomfield, R. Resanovic, Andrzej Cichocki, and H. Önel

Subjects
Physics, Cosmic Vision, Spectrometer, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, First light, Solar physics, law.invention, Telescope, Orbiter, Imaging spectroscopy, Optics, law, business
Abstract

The Spectrometer Telescope for Imaging X-rays (STIX) is one of 10 instruments on board Solar Orbiter, a confirmed Mclass mission of the European Space Agency (ESA) within the Cosmic Vision program scheduled to be launched in 2017. STIX applies a Fourier-imaging technique using a set of tungsten grids (at pitches from 0.038 to 1 mm) in front of 32 pixelized CdTe detectors to provide imaging spectroscopy of solar thermal and non-thermal hard X-ray emissions from 4 to 150 keV. The status of the instrument reviewed in this paper is based on the design that passed the Preliminary Design Review (PDR) in early 2012. Particular emphasis is given to the first light of the detector system called Caliste-SO.

Published
2012

11. Thermal simulations of the STIX instrument for ESA solar orbiter mission

Author

Adeline Bernet, Kamil Grassmann, Luc Blecha, Svend-Marian Bauer, Hans-Peter Gröbelbauer, Olivier Limousin, Karol Severyn, Gordon J. Hurford, A. Białek, Gottfied Mann, Aline Meuris, Piotr Orleańskii, H. Önel, N. G. Arnold, Konrad Skup, Oliver Grimm, Säm Krucker, and Jerome Martignac

Subjects
Physics, Orbiter, business.industry, law, Thermal, Aerospace engineering, business, law.invention

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