Abstract
The first infrared hydrogen line observation of an H II region was Hilgeman’s (1970) study of the Brackett-γ emission from the Orion Nebula. Subsequent studies of H II regions (see, for example, review by Wynn-Williams and Becklin 1974) and of the Becklin-Neugebauer source in Orion (Penston, Allen and Hyland 1971) over the next few years generally confirmed the expectation that hydrogen recombination lines were to be found in H II regions but not in “protostellar” infrared sources. This tidy differentiation was blunted by Grasdalen’s (1976) discovery of Brackett-α emission in the Becklin-Neugebauer object. Subsequently Brackett-α or Brackett-γ emission has been detected in a significant fraction of all known compact sources in molecular clouds (see, for example, review by Wynn-Williams 1982). Recently, it has become clear that the physical conditions in the emitting regions of the compact “protostellar” sources are quite unlike those in compact H II regions and more resemble those in an outflowing extended stellar atmosphere. This distinction is reflected in the organization of this review; Section II covers the observations and theory of infrared emission from compact H II regions while Section III comprises a discussion of how these ideas are being modified in the cases where the lines are formed in stellar winds.
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Wynn-Williams, C.G. (1984). Infrared Hydrogen Emission Lines from H II Regions and ‘Protostars’. In: Kessler, M.F., Phillips, J.P. (eds) Galactic and Extragalactic Infrared Spectroscopy. Astrophysics and Space Science Library, vol 108. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7251-3_9
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DOI: https://doi.org/10.1007/978-94-009-7251-3_9
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