Formation Of Amino Acids And Nucleotide Bases In A Titan Atmosphere Simulation Experiment

Details Formation Of Amino Acids And Nucleotide Bases In A Titan Atmosphere Simulation Experiment Formation Of Amino Acids And Nucleotide Bases In A Titan Atmosphere Simulation Experiment

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.3620h&link_type=abstract

American Astronomical Society, DPS meeting #42, #36.20; Bulletin of the American Astronomical Society, Vol. 42, p.1068

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Titan has been a subject of astrobiological interest since the Voyager spacecraft first revealed the diversity of the organic chemistry occurring in the atmosphere. However, it was not until the arrival of Cassini-Huygens that the chemical complexity of Titan's atmosphere was fully appreciated. The Cassini Plasma Spectrometer (CAPS) observed negative ions with m/z values up to 10,000 u/q at 950 km [1] and positive ions with m/z up to 400 u/q [2]. CAPS has also observed O+ flowing into Titan's atmosphere [3]. While Titan's atmosphere is relatively oxygen poor compared to terrestrial planets, CO is the fourth most abundant molecule in the atmosphere (˜50 ppm). The fact that the observed O+ flux is deposited in the region now known to contain large organic molecules leads to the exciting possibility that oxygen can be incorporated into these molecules resulting in the production of prebiotic molecules.
In this work, Titan aerosol analogues (or "tholins") produced in PAMPRE, a Titan atmosphere simulation experiment, have been analyzed in a very high resolution LTQ Orbitrap mass spectrometer. These PAMPRE tholins were produced by capacitively coupled RF discharge in a mixture of N2, CH4 and CO. The tholins were found to contain 18 molecules with molecular formulae corresponding to biological amino acids and nucleotide bases. GC-MS measurements have confirmed the structure of seven: adenine, cytosine, uracil, thymine, guanine, glycine and alanine. The production of prebiotic molecules under atmospheric conditions presents a new source of prebiotic material and may increase the range of planets where life could begin.
[1] Coates AJ, et al. (2007). Geophys. Res. Lett. 34:22103- +.
[2] Crary FJ, et al. (2009). Planet. Space Sci. 57:1847- 1856.
[3] Hartle RE, et al. (2006). Geophys. Res. Lett. 33:8201-+.

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