Liquid Ethane and Methane on Titan

Details Liquid Ethane and Methane on Titan Liquid Ethane and Methane on Titan

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.2306c&link_type=abstract

American Astronomical Society, DPS meeting #40, #23.06; Bulletin of the American Astronomical Society, Vol. 40, p.428

Astronomy and Astrophysics

Astronomy

Scientific paper

Absorption coefficients for liquid methane and ethane were derived in a 1-bar nitrogen atmosphere at 90K. Ethane and methane were condensed in an aluminum sample cup, and a 2-way transmission spectrum was measured. Different path lengths up to 14 mm allowed a wide range of absorption coefficients to be measured, and covered the range needed to compare to spectra of Titan in the 1- to 5-micron atmospheric windows. The data were used to compute possible liquid absorption in spectra from the Cassini Visual and Infrared Mapping Spectrometer (VIMS) and were compared to global VIMS data for Titan. The laboratory data show that both liquid methane and ethane have a strong absorption band near 4.97 microns that is detectable by VIMS. A liquid lake thickness of 3 mm (6 mm path length) would result in an absorption band depth of about 65% for methane and 85% for ethane. Ethane has a 2.02-micron absorption with a strength similar to the 4.97-micron absorption, and methane has an absorption that is 10x weaker. Continuum absorption would result in the following surface reflectance levels (at VIMS wavelengths and resolution). Examining VIMS Titan data, we find that for most of the surface, we detect no liquid methane or ethane. In a few locations VIMS data indicate liquid methane or ethane, but at less than about 1-mm total path length.

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