Chemistry in the Envelopes around Massive Young Stars

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dc.creatorvan Dishoeck, Ewine F.
dc.creatorvan der Tak, Floris F. S.
dc.date2000-02-04
dc.date.accessioned2026-07-07T01:52:07Z
dc.date.available2026-07-07T01:52:07Z
dc.descriptionRecent 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.
dc.description16 pages, 6 figures, to be published in IAU Symposium 197, Astrochemistry: from Molecular Clouds to Planetary Systems, eds. Y.C. Minh and E.F. van Dishoeck, ASP (uses newpasp.sty)
dc.identifierhttps://arxiv.org/abs/astro-ph/0002098
dc.identifierhttp://arxiv.org/abs/astro-ph/0002098
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/515
dc.subjectAstrophysics
dc.titleChemistry in the Envelopes around Massive Young Stars
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