Other
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p33a1438c&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P33A-1438
Other
1060 Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008), 6295 Venus
Scientific paper
The extreme Venus surface temperature (740K) and atmospheric pressure (93 atm) creates a challenging environment for future lander missions. The scientific investigations capable of Venus geochemical observations must be completed within several hours of the landing before the lander will be overcome by the harsh atmosphere. A combined remote Raman - LIBS (Laser Induced Breakdown Spectroscopy) instrument is capable of accomplishing the geochemical science goals without the risks associated with collecting samples and bringing them into the lander. Raman and LIBS are highly complementary analytical techniques where Raman spectroscopy is used to determine the sample molecular structure and LIBS is employed to quantitatively determine the elemental composition. Wiens et al. (2005) and Sharma et al. (2006) demonstrated that one can integrate both analytical techniques into a single instrument capable of planetary missions. Here, we will present data that demonstrates the utility of both Raman spectroscopy and LIBS under Venus conditions using separate instruments. All of the samples in these experiments were placed in a pressure vessel containing 93 atm of CO2 at 150°C and the vessel was placed 1.6m from the telescope. The elemental analysis was completed with a dual pulsed (DP) LIBS instrument employing two Nd:YAG lasers operating at 1064nm. These lasers were focused onto the sample surface and the emission was collected with a Catalina Scientific Echelle Spectrometer connected to an intensified charge coupled device (ICCD). These experiments involved probing several rock powder standards and minerals. The LIBS elemental analysis involved generating a partial least squares (PLS) model with the rock powder standards to quantitatively determine the major elemental abundance. The Raman spectra of minerals were collected up to 970 K at 9 m with a frequency doubled Nd:YAG laser operating at 532nm and the backscattered light was collected with a transmission spectrometer connected to another ICCD with 2 μs gate during daytime. A comparison of Raman spectra of gypsum (CaSO4.2H2O), dolomite (CaMg(CO3))2), olivine (Mg2Fe2-xSiO4) as a function of temperature shows that the Raman lines remains sharp and well defined even in the high temperature spectra. These time-resolved Raman measurements show that high temperature of minerals will not be a limitation and remote Raman spectroscopy would be a potential tool for rapidly exploring Venus surface mineralogy and surface processes.
Barefield James E.
Clegg Samuel M.
Misra Anupam K.
Sharma Subodh K.
Wiens Roger C.
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