Apollo 15 and 16 results of the integrated geochemical experiment

Adler, I.; Trombka, J. I.; Lowman, Paul D.; Schmadebeck, R.; Blodget, H. W.; Eller, E.; Yin, L.; Lamothe, R.; Osswald, G.; Gerard, J.; Gorenstein, P.; Bjorkholm, P.; Gursky, H.; Harris, Benjamin T; Arnold, J. R.; Metzger, A. E.; Reedy, R. C.

doi:10.1007/bf00564649

Cited by 28 publications

(8 citation statements)

References 5 publications

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“…The reflection of solar radiation was observed from the lunar orbit with Luna 12 (Mandel'shtam et al 1968), Apollo 15 and 16 (e.g. Adler et al 1973) and more recently with SMART‐1/D‐CIXS (Grande et al 2007). The black dotted line in Fig.…”

Section: Discussionmentioning

confidence: 99%

Earth X-ray albedo for cosmic X-ray background radiation in the 1–1000 keV band

Churazov¹,

Sazonov²,

Sunyaev³

et al. 2008

Monthly Notices RAS

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We present calculations of the reflection of the cosmic X‐ray background (CXB) by the Earth's atmosphere in the 1–1000 keV energy range. The calculations include Compton scattering and X‐ray fluorescent emission and are based on a realistic chemical composition of the atmosphere. Such calculations are relevant for CXB studies using the Earth as an obscuring screen (as was recently done by INTEGRAL). The Earth's reflectivity is further compared with that of the Sun and the Moon – the two other objects in the Solar system subtending a large solid angle on the sky, as needed for CXB studies.

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Section: Discussionmentioning

confidence: 99%

Earth X-ray albedo for cosmic X-ray background radiation in the 1–1000 keV band

Churazov¹,

Sazonov²,

Sunyaev³

et al. 2008

Monthly Notices RAS

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“…The sample is from Station 4A in the vicinity of Cinco B crater, 1-2 km downslope from Stone Mountain (Graf, 1993). 64 500 has been well characterized (e.g., Papike et al, 1982;McKay et al, 1991) and the Apollo 16 site is considered more homogeneous than other Apollo sites (Houck, 1982), and representative of highland regions (Adler et al, 1973). Size fraction target ranges for 64 500 are based on data from Houck (1982), Morris et al (1986), and Simon et al (1981), as well as highland data from Allton et al (1985).…”

Section: Standards and Crushing Protocolsmentioning

confidence: 99%

The Shawmere anorthosite and OB-1 as lunar highland regolith simulants

Battler

Spray

2009

Planetary and Space Science

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“…The fluorescent X‐rays can be detected by an orbiting XRS, and this information, combined with knowledge of the highly variable [e.g., Donnelly , 1976; Bouwer , 1983; Crosby et al , 1993] incident solar X‐ray spectrum (usually measured by an accompanying solar monitor), allows quantitative estimates of major rock‐forming elemental abundance ratios in the surface material to be made. X‐ray spectrometers have been included as part of the payloads on several missions to the Moon (e.g., Apollo 15 and 16 [ Adler et al , 1973], SMART‐1 [ Grande et al , 2007; Swinyard et al , 2009], SELENE [ Okada et al , 2002], and Chandrayaan‐1 [ Narendranath et al , 2011; Weider et al , 2012]); asteroids (NEAR‐Shoemaker [ Trombka et al , 2000; Nittler et al , 2001; Foley et al , 2006; Lim and Nittler , 2009], and Hayabusa [ Okada et al , 2006]); and now Mercury with the MESSENGER X‐Ray Spectrometer (XRS) [ Nittler et al , 2011] and the instrument in development for the future BepiColombo mission [ Fraser et al , 2010].…”

Section: Messenger X‐ray Spectrometermentioning

confidence: 99%

Chemical heterogeneity on Mercury's surface revealed by the MESSENGER X‐Ray Spectrometer

Weider¹,

Nittler²,

Starr³

et al. 2012

J. Geophys. Res.

159

177

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[1] We present the analysis of 205 spatially resolved measurements of the surface composition of Mercury from MESSENGER's X-Ray Spectrometer. The surface footprints of these measurements are categorized according to geological terrain. Northern smooth plains deposits and the plains interior to the Caloris basin differ compositionally from older terrain on Mercury. The older terrain generally has higher Mg/Si, S/Si, and Ca/Si ratios, and a lower Al/Si ratio than the smooth plains. Mercury's surface mineralogy is likely dominated by high-Mg mafic minerals (e.g., enstatite), plagioclase feldspar, and lesser amounts of Ca, Mg, and/or Fe sulfides (e.g., oldhamite). The compositional difference between the volcanic smooth plains and the older terrain reflects different abundances of these minerals and points to the crystallization of the smooth plains from a more chemically evolved magma source. High-degree partial melts of enstatite chondrite material provide a generally good compositional and mineralogical match for much of the surface of Mercury. An exception is Fe, for which the low surface abundance on Mercury is still higher than that of melts from enstatite chondrites and may indicate an exogenous contribution from meteoroid impacts.

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Apollo 15 and 16 results of the integrated geochemical experiment

Cited by 28 publications

References 5 publications

Earth X-ray albedo for cosmic X-ray background radiation in the 1–1000 keV band

Earth X-ray albedo for cosmic X-ray background radiation in the 1–1000 keV band

The Shawmere anorthosite and OB-1 as lunar highland regolith simulants

Chemical heterogeneity on Mercury's surface revealed by the MESSENGER X‐Ray Spectrometer

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