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1. First light observations of the solar wind in the outer corona with the Metis coronagraph

Author

F. Reale, Giuseppe Tondello, Daniele Telloni, P. Zuppella, Jean-Claude Vial, D. Moses, Luca Teriaca, Giampiero Naletto, Marco Romoli, Petr Heinzel, Federico Landini, Piergiorgio Nicolosi, Udo Schühle, Michela Uslenghi, Maurizio Pancrazzi, Silvano Fineschi, Rita Ventura, Leonard Strachan, Raffaella D'Amicis, Alessandro Liberatore, Christina Plainaki, Mauro Messerotti, Enrico Magli, Marco Stangalini, C.A. Volpicelli, Roberto Bruno, Alessandro Bemporad, Giuseppe Massone, F. Frassetto, R. Aznar Cuadrado, A. Berlicki, F. Auchere, Paolo Romano, G. Capuano, A. M. Malvezzi, Silvio Giordano, Y. De Leo, V. Da Deppo, T. Straus, Kanaris Tsinganos, Alessandra Slemer, Sami K. Solanki, Hardi Peter, V. Andretta, Cooper Downs, Daniele Spadaro, Gerardo Capobianco, A. C. Lanzafame, Gianalfredo Nicolini, Roberto Susino, Clementina Sasso, L. Zangrilli, Marco Velli, M. Casti, E. Antonucci, Angela Ciaravella, Giuseppe Nisticò, Catia Grimani, Lucia Abbo, G. Jerse, M. Fabi, Federica Frassati, Luca Poletto, Philippe Lamy, Y. M. Wang, Joachim Woch, M. G. Pelizzo, G. Zimbardo, Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Capodimonte (OAC), Università degli studi di Catania [Catania], INAF - Osservatorio Astrofisico di Catania (OACT), CNR Istituto di Fotonica e Nanotecnologie [Padova] (IFN), Consiglio Nazionale delle Ricerche [Roma] (CNR), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Predictive Sciences Inc., INAF - Osservatorio Astrofisico di Torino (OATo), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Università degli studi di Torino (UNITO), Universita degli Studi di Padova, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Naval Research Laboratory (NRL), Catholic University of America, Università degli Studi di Urbino 'Carlo Bo', Università degli studi di Trieste, Politecnico di Torino = Polytechnic of Turin (Polito), NASA Headquarters, Institute of Electronics, Computer and Telecommunication Engineering (IEIIT-CNR), Politecnico di Torino = Polytechnic of Turin (Polito)-Consiglio Nazionale delle Ricerche [Torino] (CNR), Agenzia Spaziale Italiana (ASI), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute [Wroclaw], University of Wrocław [Poland] (UWr), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), INAF - Osservatorio Astronomico di Palermo (OAPa), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Università di Pavia, Università della Calabria [Arcavacata di Rende] (Unical), Università degli studi di Palermo - University of Palermo, National and Kapodistrian University of Athens (NKUA), University of California [Los Angeles] (UCLA), University of California, Romoli M., Antonucci E., Andretta V., Capuano G.E., Da Deppo V., De Leo Y., Downs C., Fineschi S., Heinzel P., Landini F., Liberatore A., Naletto G., Nicolini G., Pancrazzi M., Sasso C., Spadaro D., Susino R., Telloni D., Teriaca L., Uslenghi M., Wang Y.-M., Bemporad A., Capobianco G., Casti M., Fabi M., Frassati F., Frassetto F., Giordano S., Grimani C., Jerse G., Magli E., Massone G., Messerotti M., Moses D., Pelizzo M.-G., Romano P., Schuhle U., Slemer A., Stangalini M., Straus T., Volpicelli C.A., Zangrilli L., Zuppella P., Abbo L., Auchere F., Aznar Cuadrado R., Berlicki A., Bruno R., Ciaravella A., D'amicis R., Lamy P., Lanzafame A., Malvezzi A.M., Nicolosi P., Nistico G., Peter H., Plainaki C., Poletto L., Reale F., Solanki S.K., Strachan L., Tondello G., Tsinganos K., Velli M., Ventura R., Vial J.-C., Woch J., and Zimbardo G.

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Solar wind, FOS: Physical sciences, Astrophysics, 01 natural sciences, Wind speed, law.invention, symbols.namesake, Sun: corona – solar wind – Sun: UV radiation, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Coronagraph, Solar and Stellar Astrophysics (astro-ph.SR), 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], Sun: corona, Astronomy and Astrophysics, Plasma, Solar wind, Sun: corona, Sun: UV radiation, Sun: UV radiation, Corona, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Temporal resolution, Physics::Space Physics, symbols, Outflow, Doppler effect
Abstract

In this work, we present an investigation of the wind in the solar corona that has been initiated by observations of the resonantly scattered ultraviolet emission of the coronal plasma obtained with UVCS-SOHO, designed to measure the wind outflow speed by applying Doppler dimming diagnostics. Metis on Solar Orbiter complements the UVCS spectroscopic observations that were performed during solar activity cycle 23 by simultaneously imaging the polarized visible light and the H I Lyman-α corona in order to obtain high spatial and temporal resolution maps of the outward velocity of the continuously expanding solar atmosphere. The Metis observations, taken on May 15, 2020, provide the first H I Lyman-α images of the extended corona and the first instantaneous map of the speed of the coronal plasma outflows during the minimum of solar activity and allow us to identify the layer where the slow wind flow is observed. The polarized visible light (580–640 nm) and the ultraviolet H I Lyα (121.6 nm) coronal emissions, obtained with the two Metis channels, were combined in order to measure the dimming of the UV emission relative to a static corona. This effect is caused by the outward motion of the coronal plasma along the direction of incidence of the chromospheric photons on the coronal neutral hydrogen. The plasma outflow velocity was then derived as a function of the measured Doppler dimming. The static corona UV emission was simulated on the basis of the plasma electron density inferred from the polarized visible light. This study leads to the identification, in the velocity maps of the solar corona, of the high-density layer about ±10° wide, centered on the extension of a quiet equatorial streamer present at the east limb – the coronal origin of the heliospheric current sheet – where the slowest wind flows at about 160 ± 18 km s−1 from 4 R⊙ to 6 R⊙. Beyond the boundaries of the high-density layer, the wind velocity rapidly increases, marking the transition between slow and fast wind in the corona.

Published
2021
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2. The Solar Orbiter Heliospheric Imager (SoloHI)

Author

J. J. Cerullo, Dennis Wang, Simon Plunkett, P. L. Lamy, S. Yerushalmi, A. P. Rouillard, J.-P. Halain, A. Thernisien, R. Baugh, D. H. Chua, R. A. Howard, Guillermo Stenborg, Robin C. Colaninno, M. T. Carter, Samuel Tun-Beltran, Spiros Patsourakos, R. Hagood, F. Auchere, Angelos Vourlidas, Sean Lynch, Dennis G. Socker, Richard A. Harrison, L. Smith, Volker Bothmer, Holly Gilbert, Greg Clifford, James Robert Janesick, Pierre Rochus, Mark Grygon, Clarence M. Korendyke, S. Koss, D. R. McMullin, Marco Velli, O. C. St. Cyr, A. Uhl, C. Mariano, P. C. Liewer, H. Dennison, K. Eisenhauer, N. Rich, T. Hunt, Jon A. Linker, Mark G. Linton, David Keller, John Robertson Tower, Adam Thurn, H. M. Maldonado, R. Farkas, Naval Research Laboratory (NRL), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Space Systems Research Corporation (SSRC), Silver Engineering, Inc., SRI International, Stinger Ghaffarian Technologies, Inc. (SGT, Inc.), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), University of California [Los Angeles] (UCLA), University of California (UC), Predictive Sciences Inc., Georg-August-University = Georg-August-Universität Göttingen, Centre Spatial de Liège (CSL), Université de Liège, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), 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), University of Ioannina, NASA Goddard Space Flight Center (GSFC), ASRC Federal Space and Defense, University of California, Georg-August-University [Göttingen], European Space Agency (ESA), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-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-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and 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)

Subjects
Physics, Zodiacal light, 010504 meteorology & atmospheric sciences, Data products, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], zodiacal dust, Sun, Astronomy and Astrophysics, telescopes, Astrophysics, Solar physics, 01 natural sciences, law.invention, Orbiter, Space and Planetary Science, law, 0103 physical sciences, Thermal, space vehicles, Aerospace engineering, business, 010303 astronomy & astrophysics, corona, 0105 earth and related environmental sciences
Abstract

Aims. We present the design and pre-launch performance of the Solar Orbiter Heliospheric Imager (SoloHI) which is an instrument prepared for inclusion in the ESA/NASA Solar Orbiter mission, currently scheduled for launch in 2020.Methods. The goal of this paper is to provide details of the SoloHI instrument concept, design, and pre-flight performance to give the potential user of the data a better understanding of how the observations are collected and the sources that contribute to the signal.Results. The paper discusses the science objectives, including the SoloHI-specific aspects, before presenting the design concepts, which include the optics, mechanical, thermal, electrical, and ground processing. Finally, a list of planned data products is also presented.Conclusions. The performance measurements of the various instrument parameters meet or exceed the requirements derived from the mission science objectives. SoloHI is poised to take its place as a vital contributor to the science success of the Solar Orbiter mission.

Published
2020
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3. The extreme UV imager of solar orbiter: from detailed design to flight model (Orale)

Author

P. Rochus, Udo Schühle, F. Auchere, Louise K. Harra, Lionel Jacques, Philip J. Smith, M. Gyo, Raymond Mercier, Laurence Rossi, C. Dumesnil, J. Tandy, Francis Verbeeck, K. Heerlein, F. Delmotte, Werner Schmutz, R. Aznar Cuadrado, S. Meining, Michel Thome, Etienne Renotte, Aline Hermans, Jean-Philippe Halain, Andrei Zhukov, Berend Winter, David Berghmans, T. Kennedy, Alexandra Mazzoli, Centre Spatial de Liège (CSL), Université de Liège, 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), Royal Observatory of Belgium [Brussels] (ROB), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Physikalisch-Meteorologisches Observatorium Davos/World Radiation Center (PMOD/WRC), Laboratoire Charles Fabry / Optique XUV, Laboratoire Charles Fabry (LCF), Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS), Takahashi, DenHerder, JWA, Bautz, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)

Subjects
Computer science, telescope, 7. Clean energy, metal filter, law.invention, Telescope, Orbiter, law, Calibration, baffle, Aerospace engineering, Extreme Ultraviolet Imager, Ultraviolet radiation, Remote sensing, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], business.industry, door mechanism, Breadboard, multilayer coating, CMOS-APS camera, Vacuum ultraviolet, Extreme ultraviolet, Solar Orbiter, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Lyman-alpha
Abstract

International audience; The Extreme Ultraviolet Imager (EUI) on-board the Solar Orbiter mission will provide full-sun and high-resolution image sequences of the solar atmosphere at selected spectral emission lines in the extreme and vacuum ultraviolet. After the breadboarding and prototyping activities that focused on key technologies, the EUI project has completed the design phase and has started the final manufacturing of the instrument and its validation. The EUI instrument has successfully passed its Critical Design Review (CDR). The process validated the detailed design of the Optical Bench unit and of its sub-units (entrance baffles, doors, mirrors, camera, and filter wheel mechanisms), and of the Electronic Box unit. In the same timeframe, the Structural and Thermal Model (STM) test campaign of the two units have been achieved, and allowed to correlate the associated mathematical models. The lessons learned from STM and the detailed design served as input to release the manufacturing of the Qualification Model (QM) and of the Flight Model (FM). The QM will serve to qualify the instrument units and sub-units, in advance of the FM acceptance tests and final onground calibration.

Published
2014
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4. Single and multi-channel Al-based multilayer systems for space applications in EUV range (Orale)

Author

Françoise Varniere, Evgueni Meltchakov, F. Delmotte, Raymond Mercier, Marc Roulliay, Xiaxiang Zhang, F. Auchere, Arnaud Jérôme, S. de Rossi, Laboratoire Charles Fabry / Optique XUV, Laboratoire Charles Fabry (LCF), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS)-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Institut d'Optique Graduate School (IOGS), Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut des Sciences Moléculaires d'Orsay (ISMO), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-Institut d'Optique Graduate School (IOGS)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Fabrication, Materials science, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Annealing (metallurgy), Extreme ultraviolet lithography, 02 engineering and technology, 7. Clean energy, 01 natural sciences, 010309 optics, chemistry.chemical_compound, Optics, 0103 physical sciences, Silicon carbide, ComputingMilieux_MISCELLANEOUS, [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], business.industry, 021001 nanoscience & nanotechnology, Solar physics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Wavelength, Optical coating, chemistry, Extreme ultraviolet, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Optoelectronics, 0210 nano-technology, business
Abstract

We report on further development of reflective mult ilayer coatings containing aluminum as low absorbin g material for the extreme ultra-violet (EUV) applications, in par ticular for solar physics. Optimizations of the mul tilayer design and deposition process have allowed us to produce Al-ba sed multilayers having relatively low interface rou ghness and record EUV reflectances in the range from 17 to 40 nm. The peak reflectance values of 56 % at 17.5 nm, 50 % a t around 21 nm, and 42 % at 32 nm were achieved with new three-material multilayers Al/Mo/SiC and Al/Mo/B 4C at near-normal incidence. We observe a good temporal stability of optical parameters of the multilayers over the peri od of 4 years. Moreover, the multilayer structure remains stable u pon annealing at 100 °C in air during several weeks . We will discuss the optical properties of more comp lex Al-based systems with regard to the design of m ultilayer coatings that reflect more than one wavelength and reject so me others within the spectral range from 17 to 40 n m. Such multichannel systems with enhanced reflectance and selec tivity would provide a further advance in optical p erformance and compactness of EUV solar imaging instruments. We will discuss general aspects of design, optimization and fabrication of single- and multi-channel multilayer mirrors mad e with the use of aluminum. We will present recent results on the EUV reflectivity of multilayer coatings based on th e Al/Mo/SiC and Al/Mo/B 4C material combinations. Al-based multilayer systems are proposed as optical coatings in EUV telescopes of future space missions and in other EUV applications.

Published
2013
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5. LEMUR: Large European Module for solar Ultraviolet Research

Author

L. Teriaca, V. Andretta, F. Auchere, C.M. Brown, E. Buchlin, G. Cauzzi, J.L. Culhane, W. Curdt, J.M. Davila, G. Del Zanna, G.A. Doschek, S. Fineschi, A. Fludra, P.T. Gallagher, L. Green, L.K. Harra, S. Imada, D. Innes, B. Kliem, C. Korendyke, J.T. Mariska, V. Mart?nez-Pillet, S. Parenti, S. Patsourakos, H. Peter, L. Poletto, R. Rutten, U. Schuehle, M. Siemer, T. Shimizu, H. Socas-Navarro, S.K. Solanki, D. Spadaro, J. Trujillo-Bueno, S. Tsuneta, S. Vargas Dominguez, J.-C. Vial, R. Walsh. H.P. Warren, T. Wiegelmann, B. Winter, and P. Young

Abstract

The solar outer atmosphere is an extremely dynamic environment characterized by the continuous interplay between the plasma and the magnetic field that generates and permeates it. Such interactions play a fundamental role in hugely diverse astrophysical systems, but occur at scales that cannot be studied outside the solar system. Understanding this complex system requires concerted, simultaneous solar observations from the visible to the vacuum ultraviolet (VUV) and soft X-rays, at high spatial resolution (between 0.1'' and 0.3''), at high temporal resolution (on the order of 10 s, i.e., the time scale of chromospheric dynamics), with a wide temperature coverage (0.01 MK to 20 MK, from the chromosphere to the flaring corona), and the capability of measuring magnetic fields through spectropolarimetry at visible and near-infrared wavelengths. Simultaneous spectroscopic measurements sampling the entire temperature range are particularly important. These requirements are fulfilled by the Japanese Solar-C mission (Plan B), composed of a spacecraft in a geosynchronous orbit with a payload providing a significant improvement of imaging and spectropolarimetric capabilities in the UV, visible, and near-infrared with respect to what is available today and foreseen in the near future. The Large European Module for solar Ultraviolet Research (LEMUR), described in this paper, is a large VUV telescope feeding a scientific payload of high-resolution imaging spectrographs and cameras. LEMUR consists of two major components: a VUV solar telescope with a 30 cm diameter mirror and a focal length of 3.6 m, and a focal-plane package composed of VUV spectrometers covering six carefully chosen wavelength ranges between 170 and 1270 . The LEMUR slit covers 280'' on the Sun with 0.14'' per pixel sampling. In addition, LEMUR is capable of measuring mass flows velocities (line shifts) down to 2 km s (-aEuro parts per thousand 1) or better. LEMUR has been proposed to ESA as the European contribution to the Solar C mission.

Published
2012
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6. Solar magnetism eXplorer (SolmeX). Exploring the magnetic field in the upper atmosphere of our closest star

Author

N.-E. Raouafi, Sami K. Solanki, Bernd Inhester, Dominik Quantius, Andy Braukhane, Luca Teriaca, D. Moses, Oliver Romberg, V. Martínez Pillet, Hansjörg Dittus, John C. Raymond, Andreas Lagg, Silvano Fineschi, Andrzej Fludra, Véronique Bommier, Jean-Claude Vial, Douglas Griffin, S. Parenti, R. Manso Sainz, Werner Curdt, Francesco Berrilli, A. Pietarila, P. Rochus, J. Trujillo Bueno, Volker Maiwald, Steven Tomczyk, Markus Schlotterer, V. Andretta, Sarah A. Matthews, E. Landi Degl'Innocenti, Joseph M. Davila, Lucia Abbo, Achim Gandorfer, Alessandro Bemporad, F. Auchere, Udo H. Schuehle, Roberto Casini, Hardi Peter, and Daniele Spadaro

Subjects
ESA Cosmic Vision, Magnetism, Solar eclipse, Extreme ultraviolet lithography, Astrophysics, 01 natural sciences, 7. Clean energy, 010309 optics, Atmosphere, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Space vehicles: instruments, 010303 astronomy & astrophysics, Physics, Spacecraft, business.industry, Sun: atmosphere, Magnetic fields, Space vehicles: instruments , Techniques: polarimetic, ESA Cosmic Vision, Sun: atmosphere - Magnetic fields - Space vehicles: instruments - Techniques: polarimetic - ESA Cosmic Vision - Concurrent Engineering, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Polarization (waves), Corona, Magnetic field, Techniques: polarimetic, Space and Planetary Science, Magnetic fields, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Sun: atmosphere
Abstract

The magnetic field plays a pivotal role in many fields of Astrophysics. This is especially true for the physics of the solar atmosphere. Measuring the magnetic field in the upper solar atmosphere is crucial to understand the nature of the underlying physical processes that drive the violent dynamics of the solar corona -- that can also affect life on Earth. SolmeX, a fully equipped solar space observatory for remote-sensing observations, will provide the first comprehensive measurements of the strength and direction of the magnetic field in the upper solar atmosphere. The mission consists of two spacecraft, one carrying the instruments, and another one in formation flight at a distance of about 200m carrying the occulter to provide an artificial total solar eclipse. This will ensure high-quality coronagraphic observations above the solar limb. Solmex integrates two spectro-polarimetric coronagraphs for off-limb observations, one in the EUV and one in the IR, and three instruments for observations on the disk. The latter comprises one imaging polarimeter in the EUV for coronal studies, a spectro-polarimeter in the EUV to investigate the low corona, and an imaging spectro-polarimeter in the UV for chromospheric studies. SOHO and other existing missions have investigated the emission of the upper atmosphere in detail (not considering polarization), and as this will be the case also for missions planned for the near future. Therefore it is timely that SolmeX provides the final piece of the observational quest by measuring the magnetic field in the upper atmosphere through polarimetric observations.

Published
2011

7. The Ultraviolet and Visible-light Coronagraph of the HERSCHEL experiment

Author

L. Zangrilli, Giampiero Naletto, A. Gherardi, Jean-Pierre Delaboudiniere, Ester Antonucci, Jeffrey S. Newmark, Silvano Fineschi, Federico Landini, R. A. Howard, M. G. Pelizzo, Marco Romoli, F. Auchere, Piergiorgio Nicolosi, Daniele Gardiol, John D. Moses, V. Da Deppo, Luca Gori, Marco Malvezzi, and Emanuele Pace

Subjects
Physics, business.industry, Stray light, Astronomy, Coronal loop, solar system, Corona, Helium, straylight, law.invention, Solar cycle, Solar wind, Optics, law, Extreme ultraviolet Imaging Telescope, Coronal mass ejection, Solar radiation, business, Coronagraph
Abstract

The Herschel (HElium Resonant Scattering in the Corona and HELiosphere) experiment, to be flown on a sounding rocket, will investigate the helium coronal abundance and the solar wind acceleration from a range of solar source structures by obtaining the first simultaneous observations of the electron, proton and helium solar corona. The HERSCHEL payload consists of the EUV Imaging Telescope (EIT), that resembles the SOHO/EIT instrument, and the Ultraviolet and Visible Coronagraph (UVC).UVC is an imaging coronagraph that will image the solar corona from 1.4 to 4 solar radii in the EUV lines of HI 121.6 nm and the HeII 30.4 nm and in the visible broadband polarized brightness. The UVC coronagraph is externally occulted with a novel design as far as the stray light rejection is concerned. Therefore, HERSCHEL will also establish proof‐of‐principle for the Ultraviolet Coronagraph, which is in the ESA Solar Orbiter Mission baseline.The scientific objectives of the experiment will be discussed, togetherwith a description of the UVC coronagraph.

Published
2003

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

Author

J. Lilensten, T. Dudok de Wit, M. Kretzschmar, P.-O. Amblard, S. Moussaoui, J. Aboudarham, and F. Auchère

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
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
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9. Recommendation for a set of solar EUV lines to be monitored for aeronomy applications

Author

J. Lilensten, T. Dudok de Wit, P.-O. Amblard, J. Aboudarham, F. Auchère, and M. Kretzschmar

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
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
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10. From the Sun to the Earth: impact of the 27-28 May 2003 solar events on the magnetosphere, ionosphere and thermosphere

Author

C. Hanuise, J. C. Cerisier, F. Auchère, K. Bocchialini, S. Bruinsma, N. Cornilleau-Wehrlin, N. Jakowski, C. Lathuillère, M. Menvielle, J.-J. Valette, N. Vilmer, J. Watermann, and P. Yaya

Subjects
Science, Physics, QC1-999, Geophysics. Cosmic physics, QC801-809
Abstract

During the last week of May 2003, the solar active region AR 10365 produced a large number of flares, several of which were accompanied by Coronal Mass Ejections (CME). Specifically on 27 and 28 May three halo CMEs were observed which had a significant impact on geospace. On 29 May, upon their arrival at the L1 point, in front of the Earth's magnetosphere, two interplanetary shocks and two additional solar wind pressure pulses were recorded by the ACE spacecraft. The interplanetary magnetic field data showed the clear signature of a magnetic cloud passing ACE. In the wake of the successive increases in solar wind pressure, the magnetosphere became strongly compressed and the sub-solar magnetopause moved inside five Earth radii. At low altitudes the increased energy input to the magnetosphere was responsible for a substantial enhancement of Region-1 field-aligned currents. The ionospheric Hall currents also intensified and the entire high-latitude current system moved equatorward by about 10°. Several substorms occurred during this period, some of them - but not all - apparently triggered by the solar wind pressure pulses. The storm's most notable consequences on geospace, including space weather effects, were (1) the expansion of the auroral oval, and aurorae seen at mid latitudes, (2) the significant modification of the total electron content in the sunlight high-latitude ionosphere, (3) the perturbation of radio-wave propagation manifested by HF blackouts and increased GPS signal scintillation, and (4) the heating of the thermosphere, causing increased satellite drag. We discuss the reasons why the May 2003 storm is less intense than the October-November 2003 storms, although several indicators reach similar intensities.

Published
2006
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