LEMUR: Large European module for solar Ultraviolet Research

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• 作者：Luca Teriaca (1) teriaca@mps.mpg.de <br>Vincenzo Andretta (2) <br>Frédéric Auchère (3) <br>Charles M. Brown (4) <br>Eric Buchlin (3) <br>Gianna Cauzzi (5) <br>J. Len Culhane (6) <br>Werner Curdt (1) <br>Joseph M. Davila (7) <br>Giulio Del Zanna (8) <br>George A. Doschek (4) <br>Silvano Fineschi (9) <br>Andrzej Fludra (10) <br>Peter T. Gallagher (11) <br>Lucie Green (6) <br>Louise K. Harra (6) <br>Shinsuke Imada (12) <br>Davina Innes (1) <br>Bernhard Kliem (13) <br>Clarence Korendyke (4) <br>John T. Mariska (4) <br>Valentin Martínez-Pillet (14) <br>Susanna Parenti (15) <br>Spiros Patsourakos (16) <br>Hardi Peter (1) <br>Luca Poletto (17) <br>Robert J. Rutten (18) <br>Udo Schühle (1) <br>Martin Siemer (19) <br>Toshifumi Shimizu (12) <br>Hector Socas-Navarro (14) <br>Sami K. Solanki (1) <br>Daniele Spadaro (20) <br>Javier Trujillo-Bueno (14) <br>Saku Tsuneta (21) <br>Santiago Vargas Dominguez (6) <br>Jean-Claude Vial (3) <br>Robert Walsh (22) <br>Harry P. Warren (4) <br>Thomas Wiegelmann (1) <br>Berend Winter (6) <br>Peter Young (23)
• 关键词：Sun ; atmosphere – Space vehicles ; instruments – Techniques ; spectroscopy – ESA cosmic vision
• 刊名：Experimental Astronomy
• 出版年：2012
• 出版时间：October 2012
• 年：2012
• 卷：34
• 期：2
• 页码：273-309
• 全文大小：1.4 MB
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• 作者单位：1. Max-Planck-Institut für Sonnensystemforschung, Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany2. INAF—Osservatorio Astronomico di Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy3. Institut d’Astrophysique Spatiale, CNRS/Université Paris-Sud 11, UMR8617, Batiment 121, 91405 Orsay, France4. Space Science Division, Naval Research Laboratory, Washington, DC 20375-5320, USA5. INAF—Osservatorio Astrofisico di Arcetri, 50125 Florence, Italy6. UCL—Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey, RH5 6NT UK7. NASA—Goddard Space Flight Center, Greenbelt, MD, USA8. University of Cambridge, Wilberforce road, Cambridge, CB2 0WA UK9. INAF—Osservatorio Astronomico di Torino, 20 Strada Osservatorio, Pino Torinese, Italy10. STFC Rutherford Appleton Laboratory, Harwell Oxford, Didcot, OX11 0QX UK11. School of Physics, Trinity College Dublin, Dublin 2, Ireland12. Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210 Japan13. Institute of Physics and Astronomy, University of Potsdam, Karl-Liebknecht-Str. 24-25, Potsdam, 14476 Germany14. Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain15. Royal Observatory of Belgium, 3 Av. Circulaire, 1180 Bruxelles, Belgium16. Department of Physics-Astrogeophysics Section, University of Ioannina, GR 451 10 Ioannina, Greece17. CNR—Institute of Photonics and Nanotechnologies, Padua, Italy18. Sterrekundig Instituut Utrecht, Utrecht, The Netherlands19. DLR—Institute of Space Systems, Bremen, Germany20. INAF—Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy21. National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588 Japan22. University of Central Lancashire, Lancashire, PR1 2HE UK23. College of Science, George Mason University, 4400 University Drive, Fairfax, VA 22030-4422, USA
• ISSN：1572-9508

文摘

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???1 or better. LEMUR has been proposed to ESA as the European contribution to the Solar C mission.