Abundances of N, S, and He, and relative stellar temperatures, in low-excitation nebulae

Details Abundances of N, S, and He, and relative stellar temperatures, in low-excitation nebulae Abundances of N, S, and He, and relative stellar temperatures, in low-excitation nebulae

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...261..195m&link_type=abstract

Astrophysical Journal, Part 1, vol. 261, Oct. 1, 1982, p. 195-199. Research supported by the Alexander von Humboldt-Stiflung an

Astronomy and Astrophysics

Astrophysics

60

Abundance, Hydrogen Clouds, Nebulae, Stellar Temperature, Diffuse Radiation, Helium, Ionization, Nitrogen, Orion Nebula, Stellar Atmospheres, Sulfur

Scientific paper

The observed abundances of He+, N+, 0+, O++, S+, and S++, relative to H+, are related to the total N, S, and He abundances through theoretical models. The parameters used to determine the total abundances are observable ratios (i.e., O+/O and S+/S++), rather than theoretical quantities (ne, Te, T*, etc.). Uncertainties in the ionizing spectra of stars introduce a considerable uncertainty in the numerical value of stellar temperature to be associated with a given star, but the nebular observations usually allow a determination of the ordering of temperatures among several nebulae. Application of the method to several regions of the Orion Nebula and to various H II regions in the LMC are encouraging. The supergiant H II region NGC 604 in M33 is excited by much cooler stars than either 30 Dor in the LMC or NGC 5471 in M101, which appears to have the hottest ionizing source among the objects discussed.

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