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Photospheres of hot stars. IV - Spectral type O4
Bohannan, Bruce; Voels, Stephen A.; Hummer, David G.; Abbott, David C.
AA(Joint Institute for Laboratory Astrophysics; Colorado, University, Boulder), AB(Joint Institute for Laboratory Astrophysics; Colorado, University, Boulder), AC(München, Universität, Munich, Germany), AD(Joint Institute for Laboratory Astrophysics; Colorado, University; NIST, Boulder)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 365, Dec. 20, 1990, p. 729-737. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Early Stars, O Stars, Photosphere, Radiative Transfer, Stellar Atmospheres, Supergiant Stars, Abundance, Helium, Line Spectra, Signal To Noise Ratios, Stellar Luminosity, Stellar Mass, Stellar Spectra
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The basic stellar parameters of a supergiant (Zeta Pup) and two main-sequence stars, 9 Sgr and HD 46223, at spectral class O4 are determined using line profile analysis. The stellar parameters are determined by comparing high signal-to-noise hydrogen and helium line profiles with those from stellar atmosphere models which include the effect of radiation scattered back onto the photosphere from an overlying stellar wind, an effect referred to as wind blanketing. At spectral class O4, the inclusion of wind-blanketing in the model atmosphere reduces the effective temperature by an average of 10 percent. This shift in effective temperature is also reflected by shifts in several other stellar parameters relative to previous O4 spectral-type calibrations. It is also shown through the analysis of the two O4 V stars that scatter in spectral type calibrations is introduced by assuming that the observed line profile reflects the photospheric stellar parameters.

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