experimental studies of lunar exosphere o.i. korablev 1, a.a. petrukovich 1, e. quémerais 2, v.i....
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Experimental studies of lunar exosphere
O.I. Korablev1, A.A. Petrukovich1, E. Quémerais2, V.I. Gnedykh1, K.I. Marchenkov1
1 Space research Institute (IKI), Moscow2 LATMOS, Guyancourt, France
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Brief history• Pre-Apollo searches:
– Polarization measurements: Fessenkov, Dollfus 10-9-10 bar
– Radioccultations (Mariner 7) : <3 10-9 H; 8 10-10 He; 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
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Sodium and Potassium
Potter & Morgan 1988
Images of the lunar sodium exosphere during total lunar eclipses Mendillo et al 1999
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Sodium and Potassium II
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Mechanisms
Stern 1999
Sprague et al1992
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Mechanisms
Lucey 2009
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Stern 1999
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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
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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
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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.
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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)
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LEVUS:
• EUV channel: 55–155 nm• FUV channel: 145–315 nm• 2 PMTs: 404, 422 nm: K, Ca lines• Scanner 360°
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LEVUS optical scheme and detectors
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Detectability of exospheric components
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