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0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System PRELIMINARY RESULTS from S -161 X-RAY EXPERIMENT I

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0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System PRELIMINARY RESULTS from S -161 X-RAY EXPERIMENT I PRELIMINARY RESULTS FROM THE S -161 X-RAY FLUOmSCENCE EXPERIMENT I. Adler, J . Trombka, J. Gerard, P. Lowman, L. Yin, and H. ~lodgett,Goddard Space Flight Center, Greenbelt, Md., 20771, and P. Gorenstein, and P. Bjorkholm, American Science and Engineering, Inc . , Cambridge, Mass., 02142. The X-Ray Fluorescence Spectrometer, carried in the SIM bay of the Command Service Module was employed principally for compositional mapping of the lunar surface while in lunar orbit, and secondarily for x-ray astronomical observations during trans earth coast . The lunar surface measurements involved observations of the intensity and characteristic energy distribution of the secondary or fluorescent x-rays produced by the inter- action of solar x-rays with the lunar surface. The astronomical observations consisted of relatively long periods of measurements of x-rays from pre- selected galactic sources such as Cyg X-1 and Sco X-1 as well as from the galactic poles. The x-ray experiment was turned on 84 hours into flight during the third lunar revolution. From 84 to 102 hours G.E.T. The orbit was approximately 8 X 60 nautical miles and during this period about 2 hours of undagraded x-data was obtained. After 102 hours the orbit was circularized and main- tained at approximately 60 nautical miles until trans-earth coast. During the orbital period over 100 hours of surface measurements were made. A solar monitor detector was used for simultaneously monitoring the solar x-ray flux. The results being reported here are based on quick-look data supplied in nearly real time. The data is in the form of running sums for the seven energy channels for each of the four experiment detectors (solar inonitor, bare detector, detector with aluminum filter and detector with magnesium filter) . The data were updated at one minute intervals. Our results as presented, are somewhat degraded in terms of spatial resolution along the projected ground track since each minute represents a three degree longitudinal displacement. Ultimately the processing of prime data, obtained for 8 second intervals should yield improved spatial information. Examining the ground tracks in a direction from east to west the space- craft is seen to have overflown such features as the craters Gargarin and Tsiolkovsky the backside and eastern limb highland, the mare area Smythii, Crisium, Fecunditatis, Tranquillitatis and Serenitatis, the Haemus Mts . , the Apennines , Mare Imbrium and Oceanus Procellarium. Plots of Al/S i intensity ratios, determined from the quick-look data have been made along the various ground tracks. One can make the following observations: 1. The Al/Si intensity ratios are lowest over the Mare areas and highest over the Terrae (average of 0.67 vs. 1.13). The extremes vary from 0.58 to 1.37, a factor of over 2.3. 0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System PRELIMINARY RESULTS FROM S -161 X-RAY EXPERIMENT I. Adler 2. The Apennine region gives a value of 0.88 and the Haemus Mts. a lower average of 0.83. On the other side of the Apennines (the Archimedes Rille area) the observed value is 0.64. On either side the values from Imbrium and Serenitatis are 0.59 and 0.58. The Apennines have values in between the mare and eastern limb highlands. Plots were also made relating Al/Si intensity ratios to albedo values and gravitational profiles. Generally the higher Al/Si ratios correspond to higher albedo values. The deviations are due to identifiable surface features such as Copernican type craters. Thus it appears that one can use x-ray data to infer compositional information of areas with differing albedos. With regard to the gravity profiles we observe the lowest Al/Si intensity ratios in the regions ofgreatest positive anomalies. An effort has been made to arrive at the actual Al/Si concentrationss using an assumed model for the solar x-ray flux and various lunar soil composit ions (determined from the analysis of lunar samples) as ground truth. The results are shown in Table 1 Table 1 Calculated Al/S i Concentration Ratios Mare Serenitatis Mare Imbrium Mare Crisium Mare Tranquillitatis Mare Fecund itatis Mare Smythii Archimedes Rilles Area (to Marsh of Decay) Apennines Mts . Haemus Mts . Highlands E. of Serenitatis to 40 E. Highlands W. and S . of Crisium Highlands between Crisium and Smythii Highlands between Smythii and Tsiolkovsky Highlands E . of Fecunditat is Highlands E . of Ts iolkovsky Area N. of Schroter Is Valley Area N.E. of Schroter's Valley --Reference Materials Apollo 11, Mare Tranquillitatis Bulk Soil 0.37 Surveyor, Mare Tranquillitatis Regolith 0.35 Apollo 12, Oceanus Procellarum Average of Soils 0.325 Luna 16, Mare Fedunditatis Bulk Soil 0.416 Surveyor V11, Rim of Tycho, Regolith 0.546 Apollo 14, Fra Mauro Soils 0.413 Apollo 15, Hadley Rille-Apennines , Soils (3 preliminary) 0.379 0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System PRELIMINARY RESULTS FROM S -161 X-RAY EXPERIMENT I. Adler Apollo 11 and 12 Anorthositic Gabbros Anorthos ite Apollo 12, Noritic Material Apollo 12, Kreep Apollo 12, Dark 12013 Some general conclusions can be drawn: 1. The Al/Si ratios confirm that the highlands and Maria do indeed have different chemical and mineralogical compositions. 2. The albedo difference between highlands and Maria are at least the express ion of chemical difference. 3. The high aluminum/silicon concentration ratios of the highlands suggests they are related to the anorthositic or noritic fractions of the returned samples, while the low Al/Si concentration ratios of the Maria is consistent with the composition of the many Mare basalts anlyzes . 4. The Imbrium ejecta blanket (Fra Mauro and Alpes Formations and possibly others) may be chemically different from the highlands outside such ejecta blankets . The intensity ratios suggest that they are intermediate in aluminum content between the Maria and the ejecta highlands. 0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System .
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