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Molecular outflows from high-mass protostars

Smith, M.D. (1998) Molecular outflows from high-mass protostars. Astrophysics and Space Science, 261 (1-4). pp. 183-184. ISSN 0004-640X. (doi:10.1023/A:1002067509862) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided) (KAR id:50144)

The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided.
Official URL
http://dx.doi.org/10.1023/A:1002067509862

Abstract

The youngest protostars are obscured from direct view by a high column of molecular gas. Nevertheless, their presence is betrayed through spectacular infrared outflows. I demonstrate here that infrared spectroscopy has the potential to reveal a remarkable variety of details concerning the underlying physics. Near-infrared spectroscopic analyses of the OMC-1, DR 21 & Cepheus A outflows are discussed here. Molecular hydrogen is vibrationally excited by collisions in shock waves. In OMC-1, the ortho-para ratio has been mapped. The ratio is close to 3, suggesting efficient shock thermalisation. In DR 21, shocked (up to the first vibrational level) and fluorescent (higher v-levels) components have been successfully separated. In Cepheus A, non-LTE effects imply low densities.

Item Type: Article
DOI/Identification number: 10.1023/A:1002067509862
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Divisions: Divisions > Division of Natural Sciences > Physics and Astronomy
Depositing User: Giles Tarver
Date Deposited: 11 Aug 2015 10:23 UTC
Last Modified: 16 Nov 2021 10:20 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/50144 (The current URI for this page, for reference purposes)
Smith, M.D.: https://orcid.org/0000-0002-4289-5952
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