Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.6821p&link_type=abstract
American Astronomical Society, DPS meeting #41, #68.21
Astronomy and Astrophysics
Astronomy
Scientific paper
Purpose of this noble gas investigation was to evaluate the feasibility of in situ K-Ar radiometric age dating of Martian surface rocks by future robotic missions, such as the Mars Science Laboratory(MSL), under constraints inherent to the Martian surface and lander design. The MSL Sample Analysis at Mars(SAM) instrument has the capability to measure noble gas compositions of Martain rocks and atmosphere. We evaluate requirements for SAM to obtain adequate noble gas abundances and compositions within the current instrumental operating conditions. In particular, maximum furnace temperature is limited to 1100ºC or lower due to power supply constraints. As a simulation experiment, we analyzed three Martian shergottites and terrestrial MORB, under the same conditions afforded SAM on the Martian surface. Our results suggest that SAM noble gas recoveries might be sufficient for K-Ar age determinations. Comparing these results with previous experiments performed on Martian meteorites at NASA-JSC, we can asses the capability of Mars lander designs with a variety of Martian rock types. The noble gas composition of Martian meteorites can be difficult to interpret due to the combined signals of in situ 40K decay, shock implanted 40Ar from Martian atmosphere[2,3], and 40Ar inherited from parent magma[4,5]. These components should also be considered in interpreting lander data. A possible advantage for landers is that K concentrations reported from the Martian surface are variable and possibly quite high, a desirable trait for K-Ar age dating. Spirit APXS reports 3000-7000ppm K for most locations but in some areas, concentrations as high as 25000ppm have been observed[6,7].
[1] Bogard (2009) MaPS44, 3-14; [2] Bogard and Johnson (1983) Science221,651-654 [3] Marti et al. (1995) Science267, 1981-1984; [4] Bogard and Park (2008) MAPS43, 1113-1126. [5] Bogard et al. (2009) MAPS44, 905-923. [6] Ming et al. (2006) JGR111, E02S12. [7] Ming D.W. et al. (2008) JGR113, E12S39.
Bogard Donald D.
Garrison Daniel H.
Houston Jones Jane
Ming Douglas W.
Park Jisun
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