Theoretical Surface Brightness Distributions and Continuum Polarization of Rapidly Rotating B Stars
George Sonneborn
- Vol. 98, pp 493-496
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TLDR
In this article, the surface brightness distribution of a rapidly rotating star was investigated using detailed model atmospheres to analyze the rotational broadening of lines in the ultraviolet and visual spectral regions.Abstract:
In order that a rotating star be in hydrostatic and radiative equilibrium, the effective temperature of the stellar atmosphere must decrease between the star's poles and its equator. Wavelength differences in this “gravity darkening” have been suggested to account for the observed differences in the rotational broadening of lines in the ultraviolet and visual spectral regions (hutchings, 1976; Sonneborn and Collins, 1977). This paper investigates the problem, using detailed model atmospheres to examine the surface brightness distribution of a rapidly rotating star.read more
References
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Journal ArticleDOI
Model atmospheres for G, F, A, B, and O stars
TL;DR: In this paper, a grid of LTE model atmospheres is presented for effective temperatures ranging from 5500 to 50,000 K, for gravities from the main sequence down to the radiation pressure limit, for abundances solar, 1/10 solar, and 1/100 solar.
Journal ArticleDOI
Intrinsic Polarization of Rapidly Rotating Early-Type Stars
Journal ArticleDOI
V sin i Values in the Far Ultraviolet
TL;DR: In this paper, a simple treatment of gravity and limb darkening shows that measured V sin i values for OB stars are significantly lower for rapid rotators in the far ultraviolet than in the photographic region of the spectrum.
Journal ArticleDOI
On the wavelength dependence of rotational line broadening.
G. H. Sonneborn,G. W. Collins +1 more