On the determination of temperatures of ionizing stars in H II regions

Details On the determination of temperatures of ionizing stars in H II regions On the determination of temperatures of ionizing stars in H II regions

Mar 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.231..257v&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 231, March 15, 1988, p. 257-267.

Astronomy and Astrophysics

Astronomy

180

Gas Ionization, H Ii Regions, Hydrogen Clouds, Positive Ions, Stellar Temperature, Astronomical Catalogs, Line Spectra, Nebulae, Oxygen Ions, Sulfur

Scientific paper

Following earlier work by Shields and Searle and by Mathis, the authors define a radiation softness parameter η = (O+/O++)(S++/S+), which they recommend as a criterion of effective temperature of the ionizing star(s) of H II regions that is relatively insensitive to chemical composition and ionization conditions found in optically observed nebulae, particularly when measurements of the nebular lines of [S III] in the far red are available. A survey of the available data for giant H II regions confirms previous suggestions that, at any given oxygen abundance, the effective temperature has an upper limit (corresponding to the youngest observed main sequence) which increases with diminishing abundance.

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