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.

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Presentation transcript:

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: –Polarization measurements: Fessenkov, Dollfus  bar –Radioccultations (Mariner 7) : < H; He; Ar –Lunar Transient Phenomena Apollo –SIDE: Suprathermal ion detector: 20 Ne and 40 Ar detections –Cathode gauges: N 2 assumption: cm -3 day … cm -3 night –LACE mass spectrometer: Ar, He H 2 O, CH 4, N 2,CO, CO 2 –α-particle spectrometers (A15): 222 Rn, 210 Po –Orbital mass spectrometers (A15-16) –UV spectrometer (A17) Ground-based discovery of K and Na [Potter & Morgan 1988] Hodges 1985

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

Sodium and Potassium II

Mechanisms Stern 1999 Sprague et al1992

Mechanisms Lucey 2009

Stern 1999

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

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 UVS : 200–800 nm -NMS

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.

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)

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

LEVUS optical scheme and detectors

Detectability of exospheric components

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