HH Illumination of Clumps within Molecular Clouds

Details HH Illumination of Clumps within Molecular Clouds HH Illumination of Clumps within Molecular Clouds

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15..126w&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Other

Ism: Jets And Outflows, Ism: Molecules

Scientific paper

Molecular clouds are clumpy. Much of the clumpiness is unresolved by single-dish telescopes but is apparent in the data from array telescopes. Even in the unresolved observational data, the existence of clumpiness can be inferred from the distribution of molecular species. This evidence requires that ``early-time'' molecular species are widespread, while ``late-time'' species are more confined, and possibly associated with newly formed stars. The clumps are required to be transient.
Molecular clumps may also be observed close to HH objects. These clumps have a chemical composition different from that of clumps in a cloud interior, and the emissions from HCO+ and NH[3] are strong. These HH clumps are dynamically quiescent; they have not been overtaken by the HH shock. We discuss here a detailed observational and theoretical study of one HH clump, and show that this clump must be transient and have a similar density and temperature to those clumps detected or inferred in the cloud interior. The anomalous chemistry is shown to be the result of HH illumination of regions that would otherwise be dark, so that in these regions a significant photochemistry develops. Thus, HH clumps are probably of the same family as the clumps in cloud interiors, even though they are chemically distinct.
It is a consequence of the ideas presented here that the clump mass distribution should be related to the formation of low-mass stars.

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