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2000MNRAS.313..461R - Mon. Not. R. Astron. Soc., 313, 461-468 (2000/April-2)
A source of extended HCO+ emission in young stellar objects.
RAWLINGS J.M.C., TAYLOR S.D. and WILLIAMS D.A.
Abstract (from CDS):
This paper presents a model for the source of the HCO+ emission excess. Observations have shown that, in low-mass star-forming regions, the collapse process is invariably accompanied by the presence of collimated outflows; we therefore propose the presence of an interface region around the outflow in which the chemistry is enriched by the action of jets. This hypothesis suggests that the line profiles of HCO+, as well as other molecular species, may require a more complex interpretation than can be provided by simple, chemically quiescent, spherically symmetric infall models.
The enhancement of HCO+ depends primarily on the presence of a shock-generated radiation field in the interface. Plausible estimates of the radiation intensity imply molecular abundances that are consistent with those observed. Further, high-resolution observations of an infall-outflow source show HCO+ emission morphology that is consistent with that predicted by this model.
Abstract Copyright: 2000, Royal Astronomical Society
Journal keyword(s): stars: formation - ISM: clouds - ISM: jets and outflows - ISM: molecules
Simbad objects: 1
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