HC3N and the ages of dense cores

Details HC3N and the ages of dense cores HC3N and the ages of dense cores

Feb 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26a...354.1127g&link_type=abstract

Astronomy and Astrophysics, v.354, p.1127-1133 (2000)

Astronomy and Astrophysics

Astrophysics

14

Ism: Clouds, Ism: General, Ism: Molecules

Scientific paper

Fractional abundances of HC_3N and a number of other species are presented for dense core models based on a variety of different assumptions. The highest calculated values of the HC_3N fractional abundances arise in static models where many species striking grain surfaces are processed in hydrogenation reactions leading to the rapid injection of saturated species into the gas phase; in these models the HC_3N is most abundant well before chemical equilibrium is reached. The effects of the various parameters considered are strongly coupled and lead to markedly differing ratios of the HC_3N abundance relative to abundances of other species including H_2CO, C_3H and C_4H. Although none of these models is specific to any particular astronomical object, we briefly compare our results with abundances observed in TMC-1. We conclude that the molecular abundances observed in TMC-1 can be accounted for on the basis of models of the type discussed here, and that - although this much-studied object has unusually high molecular abundances - it is not chemically anomalous compared to other dense cores.

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