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Chemistry in the Envelopes around Massive Young Stars

Published online by Cambridge University Press:  25 May 2016

Ewine F. van Dishoeck  and
Floris F. S. van der Tak
Ewine F. van Dishoeck
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands
Floris F. S. van der Tak
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands

Abstract

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Recent observational studies of intermediate- and high-mass star-forming regions at submillimeter and infrared wavelengths are reviewed, and chemical diagnostics of the different physical components associated with young stellar objects are summarized. Procedures for determining the temperature, density and abundance profiles in the envelopes are outlined. A detailed study of a set of infrared-bright massive young stars reveals systematic increases in the gas/solid ratios, the abundances of evaporated molecules, and the fraction of heated ices with increasing temperature. Since these diverse phenomena involve a range of temperatures from < 100 K to 1000 K, the enhanced temperatures must be communicated to both the inner and outer parts of the envelopes. This ‘global heating’ plausibly results from the gradual dispersion of the envelopes with time. Similarities and differences with low-mass YSOs are discussed. The availability of accurate physical models will allow chemical models of ice evaporation followed by ‘hot core’ chemistry to be tested in detail.

Type
Part 2. Chemistry in High-Mass Star-Forming Regions
Information
Symposium - International Astronomical Union , Volume 197: Astrochemistry: From Molecular Clouds to Planetary Systems , 2000 , pp. 97 - 112
Copyright
Copyright © Astronomical Society of the Pacific 2000 

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