Models of Interstellar Anion Chemistry

Details Models of Interstellar Anion Chemistry Models of Interstellar Anion Chemistry

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541522c&link_type=abstract

American Astronomical Society, AAS Meeting #215, #415.22; Bulletin of the American Astronomical Society, Vol. 42, p.264

Biology

1

Scientific paper

Chemical models are presented for the dense, star-forming interstellar cloud L1527, which contains a class 0/I protostar and exhibits large abundances of carbon-chain-bearing molecules (including CnH, CnH-, HCnN and CH3CCH). We are able to accurately reproduce the observed chemical abundances in this cloud using standard gas-phase chemical models. The two models presented include dust grain accretion and freefall collapse of the cloud, but without the need for any sublimation of mantle ices as the protostar forms and begins to warm the surrounding cloud. Thus, we find that standard gas-phase chemical models may be used to study the chemistry of such regions, and that the so-called "warm carbon-chain chemistry" postulated by Sakai et al. (2008, ApJ, 672, 371) may be due to the presence of left-over carbon chains formed during the earlier, cooler phase of the collapsing cloud.
This work was supported by NASA's Origins of Solar Systems Program and by the Goddard Center for Astrobiology.

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