Experimental Study of Ethylene Evaporites under Titan Conditions
by Czaplinski, Ellen C.; Gilbertson, Woodrow A.; Farnsworth, Kendra K.; Chevrier, Vincent F.
Titan has an abundance of lakes and seas, as confirmed by Cassini. Major components of these liquid bodies include methane (CH4) and ethane (C2H6); however, evidence indicates that minor components such as ethylene (C2H4) may also exist in the lakes. As the lake levels drop, 5 mu m-bright deposits, resembling evaporite deposits on earth, are left behind. Here, we provide saturation values, evaporation rates, and constraints on ethylene evaporite formation by using a Titan simulation chamber capable of reproducing Titan surface conditions (89-94 K, 1.5 bar N-2). Experimental samples were analyzed using Fourier transform infrared spectroscopy, mass, and temperature readings. Ethylene evaporites form more quickly in a methane solvent than in an ethane solvent or in a mixture of methane/ ethane. We measured an average evaporation rate of (2.8 +/- 0.3) X 10(-4) kg m(-2) s(-1) for methane and an average upper limit evaporation rate of <5.5 x 10(-6) kg m(-2) s(-1) for ethane. Additionally, we observed red shifts in ethylene absorption bands at 1.630 and 2.121 mu m and the persistence of a methane band at 1.666 mu m.
- Journal
- ACS Earth and Space Chemistry
- Volume
- 3
- Issue
- 10
- Year
- 2019
- Start Page
- 2353-2362
- URL
- https://dx.doi.org/10.1021/acsearthspacechem.9b00204
- ISBN/ISSN
- 2472-3452
- DOI
- 10.1021/acsearthspacechem.9b00204