Beyond the disk: EUV coronagraphic observations of the Extreme Ultraviolet Imager on board Solar Orbiter

被引：0

作者：

Auchère, F. ^{[1
]}

Berghmans, D. ^{[2
]}

Dumesnil, C. ^{[1
]}

Halain, J.-P. ^{[3
]}

Mercier, R. ^{[4
]}

Rochus, P. ^{[3
]}

Delmotte, F. ^{[4
]}

François, S. ^{[1
]}

Hermans, A. ^{[3
]}

Hervier, V. ^{[1
]}

Kraaikamp, E. ^{[2
]}

Meltchakov, E. ^{[4
]}

Morinaud, G. ^{[1
]}

Philippon, A. ^{[1
]}

Smith, P.J. ^{[5
]}

Stegen, K. ^{[2
]}

Verbeeck, C. ^{[2
]}

Zhang, X. ^{[1
]}

Andretta, V. ^{[9
]}

Abbo, L. ^{[10
]}

Buchlin, E. ^{[1
]}

Frassati, F. ^{[10
]}

Gissot, S. ^{[2
]}

Gyo, M. ^{[6
]}

Harra, L. ^{[6
,7
]}

Jerse, G. ^{[11
]}

Landini, F. ^{[10
]}

Mierla, M. ^{[2
,13
]}

Nicula, B. ^{[2
]}

Parenti, S. ^{[1
]}

Renotte, E. ^{[3
]}

Romoli, M. ^{[12
]}

Russano, G. ^{[9
]}

Sasso, C. ^{[9
]}

Schühle, U. ^{[8
]}

Schmutz, W. ^{[6
]}

Soubrié, E. ^{[1
]}

Susino, R. ^{[10
]}

Teriaca, L. ^{[8
]}

West, M. ^{[14
]}

Zhukov, A.N. ^{[2
,15
]}

机构：

[1] Université Paris-Saclay, Cnrs, Institut d'Astrophysique Spatiale, Orsay,91405, France

[2] Solar-Terrestrial Centre of Excellence - Sidc, Royal Observatory of Belgium, Brussels, Belgium

[3] Centre Spatial de Liège, Université de Liège, Av. du Pré-Aily B29, Angleur,4031, Belgium

[4] Laboratoire Charles Fabry, Institut d'Optique Graduate School, Université Paris-Saclay, Palaiseau,91127 Cedex, France

[5] UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey,RH5 6NT, United Kingdom

[6] Physikalisch-Meteorologisches Observatorium Davos, World Radiation Center, Davos Dorf, 7260, Switzerland

[7] ETH-Zurich, Hönggerberg campus, HIT building, Zürich, Switzerland

[8] Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, Göttingen,37077, Germany

[9] Inaf - Osservatorio Astronomico di Capodimonte, Napoli, Italy

[10] Inaf - Osservatorio Astrofisico di Torino, Pino Torinese, Italy

[11] Inaf - Osservatorio Astronomico di Trieste, Basovizza, Trieste, Italy

[12] Dipartimento di Fisica e Astronomia, Università di Firenze, Florence, Italy

[13] Institute of Geodynamics of the Romanian Academy, Bucharest, Romania

[14] Southwest Research Institute, 1050 Walnut Street, Boulder,CO,80302, United States

[15] Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow,119992, Russia

来源：

Astronomy and Astrophysics | 2023年 / 674卷

关键词：

Number: -, Acronym: UCL, Sponsor: University College London, Number: 4000134474,4000136424, Acronym: ESA, Sponsor: European Space Agency, Number: BELSPO/PRODEX PEA C4000134088, Acronym: BELSPO, Sponsor: Belgian Federal Science Policy Office, Number: -, Acronym: CNES, Sponsor: Centre National d’Etudes Spatiales, Number: -, Acronym: DLR, Sponsor: Deutsches Zentrum für Luft- und Raumfahrt, Number: -, Acronym: ASI, Sponsor: Agenzia Spaziale Italiana, Number: -, Acronym: WRC, Sponsor: Water Research Commission, Number: -, Acronym: BMWi, Sponsor: Bundesministerium für Wirtschaft und Energie,;

D O I：

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中图分类号：

学科分类号：

摘要：

Context. Most observations of the solar corona beyond 2 R consist of broadband visible light imagery carried out with coronagraphs. The associated diagnostics mainly consist of kinematics and derivations of the electron number density. While the measurement of the properties of emission lines can provide crucial additional diagnostics of the coronal plasma (temperatures, velocities, abundances, etc.), these types of observations are comparatively rare. In visible wavelengths, observations at these heights are limited to total eclipses. In the ultraviolet (UV) to extreme UV (EUV) range, very few additional observations have been achieved since the pioneering results of the Ultraviolet Coronagraph Spectrometer (UVCS). Aims. One of the objectives of the Full Sun Imager (FSI) channel of the Extreme Ultraviolet Imager (EUI) on board the Solar Orbiter mission has been to provide very wide field-of-view EUV diagnostics of the morphology and dynamics of the solar atmosphere in temperature regimes that are typical of the lower transition region and of the corona. Methods. FSI carries out observations in two narrowbands of the EUV spectrum centered on 17.4 nm and 30.4 nm that are dominated, respectively, by lines of FeIX/X (formed in the corona around 1 MK) and by the resonance line of HeII (formed around 80 kK in the lower transition region). Unlike previous EUV imagers, FSI includes a moveable occulting disk that can be inserted in the optical path to reduce the amount of instrumental stray light to a minimum. Results. FSI detects signals at 17.4 nm up to the edge of its field of view (7 R), which is about twice further than was previously possible. Operation at 30.4 nm are for the moment compromised by an as-yet unidentified source of stray light. Comparisons with observations by the LASCO and Metis coronagraphs confirm the presence of morphological similarities and differences between the broadband visible light and EUV emissions, as documented on the basis of prior eclipse and space-based observations. Conclusions. The very-wide-field observations of FSI out to about 3 and 7 R, without and with the occulting disk, respectively, are paving the way for future dedicated instruments. © The Authors 2023.

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