Models of dense cores in translucent regions of low mass star formation

Details Models of dense cores in translucent regions of low mass star formation Models of dense cores in translucent regions of low mass star formation

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.220..261n&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 220, no. 2, p. 261-278

Astronomy and Astrophysics

Astrophysics

11

Abundance, Astronomical Models, Cosmic Dust, Interstellar Gas, Interstellar Radiation, Star Formation, Stellar Cores, Stellar Winds, Halley'S Comet, Radio Spectra, Spectroscopy, Stellar Temperature

Scientific paper

We have constructed models for a region of low mass star formation where stellar winds ablate material from dark dense cores and return it to a translucent intercore medium from which subsequent generations of cores condense. Depletion of gas phase species onto grains plays a major role in the chemistry. For reasonable agreement between model core chemical fractional abundances and measured TMC-1 fractional abundances to obtain, the core collapse, once started, must be relatively uninhibited by turbulence or magnetic fields and the core lifetime must fall in a limited range determined by the assumed depletion rates. In a core with the TMC-1 fractional abundances, CH, OH, C2H, H2CO, HCN, HNC, and CN are the only simple species that have been detected in TMC-1 at radio and millimeter wavelengths to have fractional abundances that are roughly constant or increasing with time; this result bears considerably on previous work concerned with searches for spectroscopic evidence for and the diagnosis of collapse during protostellar formation, but depends on the fractions of the OH and CH emissions that are associated with the core center rather than more extended gas or a core-stellar wind boundary layer. Model results for the abundance ratios of H2O, CH4, and NH3 ices are in good agreement with those inferred for Halley's Comet.

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