Abstract
Infrared atomic hydrogen lines observed in luminous stars, generally attributed to compact circumstellar HII regions, can also be formed in the winds likely to emanate from these stars. We show how the mass-loss rate may be estimated from line fluxes, and also how constraints on the velocity profile may be deduced. Winds capable of producing lines of the observed flux should also be weak, but detectable, sources of radio emission.
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Krolik, J.H., Smith, H.A. (1982). Infrared Atomic Hydrogen Line Formation in Luminous Stars. In: Roger, R.S., Dewdney, P.E. (eds) Regions of Recent Star Formation. Astrophysics and Space Science Library, vol 93. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7778-5_22
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DOI: https://doi.org/10.1007/978-94-009-7778-5_22
Publisher Name: Springer, Dordrecht
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