The BepiColombo Mercury Imaging X-Ray Spectrometer: Science Goals, Instrument Performance and Operations

被引：36

作者：

Bunce, Emma J. ^{[1
]}

Martindale, Adrian ^{[1
]}

Lindsay, Simon ^{[1
]}

Muinonen, Karri ^{[2
,3
]}

Rothery, David A. ^{[4
]}

Pearson, Jim ^{[1
]}

McDonnell, Ivor ^{[1
]}

Thomas, Chris ^{[1
]}

Thornhill, Julian ^{[1
]}

Tikkanen, Tuomo ^{[1
]}

Feldman, Charly ^{[1
]}

Huovelin, Juhani ^{[2
]}

Korpela, Seppo ^{[2
]}

Esko, Eero ^{[2
]}

Lehtolainen, Arto ^{[2
]}

Treis, Johannes ^{[5
]}

Majewski, Petra ^{[6
]}

Hilchenbach, Martin ^{[7
]}

Vaisanen, Timo ^{[2
]}

Luttinen, Arto ^{[8
]}

Kohout, Tomas ^{[9
]}

Penttila, Antti ^{[2
]}

Bridges, John ^{[1
]}

Joy, Katherine H. ^{[10
]}

Alcacera-Gil, Maria Angeles ^{[11
]}

Alibert, Guilhem ^{[12
]}

Anand, Mahesh ^{[4
]}

Bannister, Nigel ^{[1
]}

Barcelo-Garcia, Corinne ^{[12
]}

Bicknell, Chris ^{[1
]}

Blake, Oliver ^{[1
]}

Bland, Phil ^{[13
]}

Butcher, Gillian ^{[1
]}

Cheney, Andy ^{[1
]}

Christensen, Ulrich ^{[7
]}

Crawford, Tony ^{[1
]}

Crawford, Ian A. ^{[14
]}

Dennerl, Konrad ^{[15
]}

Dougherty, Michele ^{[16
]}

Drumm, Paul ^{[1
]}

Fairbend, Raymond ^{[12
]}

Genzer, Maria ^{[17
]}

Grande, Manuel ^{[18
]}

Hall, Graeme P. ^{[1
]}

Hodnett, Rosie ^{[1
]}

Houghton, Paul ^{[1
]}

Imber, Suzanne ^{[1
]}

Kallio, Esa ^{[19
]}

Lara, Maria Luisa ^{[20
]}

Balado Margeli, Ana ^{[11
]}

机构：

[1] Univ Leicester, Sch Phys & Astronomy, Univ Rd, Leicester LE1 7RH, Leics, England

[2] Univ Helsinki, Dept Phys, Gustaf Hallstromin Katu 2, Helsinki 00560, Finland

[3] Finnish Geospatial Res Inst FGI, Natl Land Survey Finland, Geodeetinrinne 2, Masala 02430, Finland

[4] Open Univ, Sch Phys Sci, Milton Keynes MK7 6AA, Bucks, England

[5] Max Planck Gesell, Semicond Lab, Otto Hahn Ring 6, D-81739 Munich, Germany

[6] PNSensor GmbH, Otto Hahn Ring 6, D-81739 Munich, Germany

[7] Max Planck Inst Solar Syst Res, Justus von Liebig Weg 3, D-37077 Gottingen, Germany

[8] Finnish Museum Nat Hist, Pohjoinen Rautatiekatu 13, Helsinki, Finland

[9] Dept Geosci & Geog, Gustaf Hallstromin Katu 2, Helsinki 00560, Finland

[10] Univ Manchester, Dept Earth & Environm Sci, Oxford Rd, Manchester M13 9PL, England

[11] Inst Nacl Tecn Aeroesp, Ctra Torrejon Ajalvir, km 4, Madrid 28850, Spain

[12] Photonis France SAS, Ave Roger Roncier, F-19100 Brive, France

[13] Curtin Univ, Fac Sci & Engn, Perth, WA 6102, Australia

[14] Birkbeck Coll Univ London, Dept Earth & Planetary Sci, London, England

[15] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[16] Imperial Coll London, Blackett Lab, London, England

[17] Finnish Meteorol Inst, Erik Palmenin Aukio 1, Helsinki 00560, Finland

[18] Aberystwyth Univ, Aberystwyth, Dyfed, Wales

[19] Aalto Univ, Sch Elect Engn, Espoo 02150, Finland

[20] Inst Astrofis Andalucia, Glorieta Astron S-N, Granada 18008, Spain

[21] CSIC INTA, Ctr Astrobiol, Ctra Torrejon Ajalvir,Km 4, Madrid 28850, Spain

[22] Inst Recherce Astrophys & Planetol, 9 Ave Colonel Roche, F-31400 Toulouse, France

[23] Oxford Instruments Technol Oy, Espoo 02150, Finland

[24] Carnegie Inst Sci, Earth & Planets Lab, 5241 Broad Branch Rd, Washington, DC 20015 USA

[25] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2998510, Japan

[26] Harvard Univ, Dept Earth & Planetary Sci, Origins Life Initiat, Cambridge, MA 02138 USA

[27] Univ Leicester, Sch Engn, Univ Rd, Leicester LE1 7RH, Leics, England

来源：

SPACE SCIENCE REVIEWS | 2020年 / 216卷 / 08期

基金：

英国科学技术设施理事会; 芬兰科学院;

关键词：

Mercury; BepiColombo; X-ray spectrometry; Surface composition; X-ray emission; Elemental composition; FLUORESCENCE; SURFACE; CALIBRATION; REGOLITH; MIXS; MECHANISMS; DETECTORS; ABUNDANCE; CRUST;

D O I：

10.1007/s11214-020-00750-2

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Mercury Imaging X-ray Spectrometer is a highly novel instrument that is designed to map Mercury's elemental composition from orbit at two angular resolutions. By observing the fluorescence X-rays generated when solar-coronal X-rays and charged particles interact with the surface regolith, MIXS will be able to measure the atomic composition of the upper similar to 10-20 mu m of Mercury's surface on the day-side. Through precipitating particles on the night-side, MIXS will also determine the dynamic interaction of the planet's surface with the surrounding space environment. MIXS is composed of two complementary elements: MIXS-C is a collimated instrument which will achieve global coverage at a similar spatial resolution to that achieved (in the northern hemisphere only - i.e. similar to 50 - 100 km) by MESSENGER; MIXS-T is the first ever X-ray telescope to be sent to another planet and will, during periods of high solar activity (or intense precipitation of charged particles), reveal the X-ray flux from Mercury at better than 10 km resolution. The design, performance, scientific goals and operations plans of the instrument are discussed, including the initial results from commissioning in space.

引用

页数：38

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