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H Atom Observations in Near-Stellar Environments

Published online by Cambridge University Press:  07 August 2017

Luis F. Rodriguez
Luis F. Rodriguez*
Affiliation:
Instituto de Astronomía, UNAM Apdo. Postal 70-264 México, DF 04510, México

Abstract

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Interferometric observations of the 21-cm line of atomic hydrogen resolve out the emission from extended, line-of-sight clouds and allow the detailed study of compact H I structures in the surroundings of some stars. These atomic hydrogen components most probably are the result of photodissociation of gas that originally was in molecular form. They have been observed in H II regions, reflection nebulae, and planetary nebulae. The study of this atomic hydrogen component is important to determine the mass and physical conditions of gas in the environment of luminous stars and to test our theoretical knowledge of photodissociation regions.

Type
Near Stellar Environments
Information
Symposium - International Astronomical Union , Volume 150: Astrochemistry of Cosmic Phenomena , 1992 , pp. 351 - 355
Copyright
Copyright © Kluwer 1992 

References

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