Physics
Scientific paper
Feb 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012georl..3904309a&link_type=abstract
Geophysical Research Letters, Volume 39, Issue 4, CiteID L04309
Physics
Mineralogy And Petrology: Planetary Mineralogy And Petrology (5410), Mineral Physics: Optical, Infrared, And Raman Spectroscopy, Planetary Sciences: Solid Surface Planets: Composition (1060, 3672), Planetary Sciences: Solid Surface Planets: Ices, Planetary Sciences: Solar System Objects: Titan
Scientific paper
Reflectance spectroscopy of outer solar system bodies provides direct observations for interpreting their surface compositions. At Titan, the Cassini spacecraft revealed dark patches in the surface reflectance at 2 and 5 μm, interpreted as hydrocarbon lakes forming seasonally through a methane cycle. Whereas the composition of planetary materials in the solar system has been inferred from characteristic absorption bands, identification of phase states (liquid versus solid) on dynamic planetary surfaces requires laboratory reflectance ratio measurements at relevant temperatures. Using visible and near-infrared radiation from the National Synchrotron Light Source (NSLS), reflectance ratios of solid (single crystal) versus liquid CH4 were measured at temperatures from 50-100 K. Although the wavelength and shape of the characteristic methane absorption bands at around 1.7 and 2.3 μm are insensitive to temperature or phase state from 50-100 K, the broad-spectrum reflectivity R(λ) at 0.5-2 μm decreases dramatically upon melting by at least 25% at 87-94 K. Transition from solid CH4-I to liquid states at ˜90 K displays a reflectance ratio Rsolid/Rliq 1.3-1.6 at 2 μm. This darkening of CH4 upon melting at 87-94 K is similar at visible wavelengths, and consistent with observations of hydrocarbon lakes in the far northern and southern latitudes of Titan.
Adams Kimberly A.
Jacobsen Steven D.
Jurdy Donna M.
Liu Zhenxian
Somayazulu Maddury
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