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Self-assembly of tholins in environments simulating Titan liquidospheres: implications for formation of primitive coacervates on Titan

Published online by Cambridge University Press:  15 May 2013

Jun Kawai ,
Seema Jagota ,
Takeo Kaneko ,
Yumiko Obayashi ,
Yoshitaka Yoshimura ,
Bishun N. Khare ,
David W. Deamer ,
Christopher P. McKay  and
Kensei Kobayashi
Jun Kawai
Affiliation:
Department of Chemistry and Biotechnology, Yokohama National University, Hodogaya-ku, Yokohama 240-8501, Japan e-mail: [email protected]
Seema Jagota
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035-1000, USA
Takeo Kaneko
Affiliation:
Department of Chemistry and Biotechnology, Yokohama National University, Hodogaya-ku, Yokohama 240-8501, Japan e-mail: [email protected]
Yumiko Obayashi
Affiliation:
Department of Chemistry and Biotechnology, Yokohama National University, Hodogaya-ku, Yokohama 240-8501, Japan e-mail: [email protected]
Yoshitaka Yoshimura
Affiliation:
Department of Life Science, Tamagawa University, Machida, Tokyo 194-8600, Japan
Bishun N. Khare
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035-1000, USA
David W. Deamer
Affiliation:
Jack Baskin School of Engineering, University of California, Santa Cruz 95064-1077, USA
Christopher P. McKay
Affiliation:
NASA Ames Research Center, Moffett Field, CA 94035-1000, USA
Kensei Kobayashi
Affiliation:
Department of Chemistry and Biotechnology, Yokohama National University, Hodogaya-ku, Yokohama 240-8501, Japan e-mail: [email protected]
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Abstract

Titan, the largest satellite of Saturn, has a thick atmosphere containing nitrogen and methane. A variety of organic compounds have been detected in the atmosphere, most likely produced when atmospheric gases are exposed to ultraviolet light, electrons captured by the magnetosphere of Saturn and cosmic rays. The Cassini/Huygens probe showed that the average temperature on the surface of Titan is 93.7 K, with lakes of liquid ethane and methane. Sub-surface mixtures of liquid ammonia and water may also be present. We have synthesized complex organic compounds (tholins) by exposing a mixture of nitrogen and methane to plasma discharges, and investigated their interactions with several different liquids that simulate Titan's liquidosphere. We found that coacervates formed when tholins were extracted in non-polar solvents followed by exposure to aqueous ammonia solutions. The results suggest that coacervates can self-assemble in Titan's liquidosphere which have the potential to undergo further chemical evolution. Similar processes are likely to occur in the early evolution of habitable planets when tholin-like compounds undergo phase separation into microscopic structures dispersed in a suitable aqueous environment.

Keywords

coacervatesliquidosphereself-assemblytholinTitan
Type
Research Article
Information
International Journal of Astrobiology , Volume 12 , Issue 4 , October 2013 , pp. 282 - 291
Copyright
Copyright © Cambridge University Press 2013 

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