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Experimental studies of lunar exosphere

Experimental studies of lunar exosphere. O.I. Korablev 1 , A.A. Petrukovich 1 , E. Quémerais 2 , V.I. Gnedykh 1 , K.I. Marchenkov 1 1 Space research Institute (IKI), Moscow 2 LATMOS, Guyancourt, France. Brief history. Pre-Apollo searches:

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Experimental studies of lunar exosphere

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  1. Experimental studies of lunar exosphere O.I. Korablev1, A.A. Petrukovich1, E. Quémerais2, V.I. Gnedykh1, K.I. Marchenkov1 1 Space research Institute (IKI), Moscow 2 LATMOS, Guyancourt, France

  2. Brief history • Pre-Apollo searches: • Polarization measurements: Fessenkov, Dollfus  10-9-10 bar • Radioccultations (Mariner 7) : <3 10-9 H; 8 10-10He; 8 10-12 Ar • Lunar Transient Phenomena • Apollo • SIDE: Suprathermal ion detector: 20Ne and 40Ar detections • Cathode gauges: N2 assumption: 2 107cm-3 day … 2 105cm-3 night • LACE mass spectrometer: Ar, He H2O, CH4, N2,CO, CO2 • α-particle spectrometers (A15): 222Rn, 210Po • Orbital mass spectrometers (A15-16) • UV spectrometer (A17) • Ground-based discovery of K and Na [Potter & Morgan 1988] Hodges 1985

  3. Sodium and Potassium Potter & Morgan 1988 Images of the lunar sodium exosphere during total lunar eclipses Mendillo et al 1999

  4. Sodium and Potassium II

  5. Mechanisms Stern 1999 Sprague et al1992

  6. Mechanisms Lucey 2009

  7. Stern 1999

  8. Recent space observations • SARA /Chandrayan-1: low energy neutral atom sensor 10 eV – 3.3 keV and ion mass spectrometer (10 eV – 15 keV) • UPI-TVIS/SELENE: UV and visible (Na D2, OI) narrow-band imager • LAMP/MRO

  9. UV-spectrometry from space • LRO/LAMP: • Spectral range 57–196 nm • Observation of the LCROSS plume • Mapping of lunar poles in L-alpha • LADEE mission: NASA 2012 • UVS : 200–800 nm • NMS

  10. UV-spectrometry from Luna Globe Orbiter LEVUS: Lunar Exosphere EUV/UV spectrometer • On the basis of PHEBUS/Bepi Colombo • French PI of PHEBUS: Eric Quémerais, 2 co-PIs • Detectors from Japan (customized Hamamatsu design) • Scanner system from IKI/Russia • LEVUS = spare of PHEBUS provided by France with interfaces and scanner modified by IKI. IKI provides all prototypes for Luna Globe.

  11. LEVUS : Science objectives • To detect/reduce upper limits of expected components of the lunar exosphere • To study the sources, sinks and transport mechanisms of exosphere species • To explore the EUV range, not covered so far • To map the surface in the UV range • To study the solar wind and its interaction with the moon • UV observatory: comets,… • Terrestrial exosphere (geocorona)

  12. LEVUS: • EUV channel: 55–155 nm • FUV channel: 145–315 nm • 2 PMTs: 404, 422 nm: K, Ca lines • Scanner 360°

  13. LEVUS optical scheme and detectors

  14. Detectability of exospheric components

  15. Back-up

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