Highly ionized stellar winds in Be stars - The evidence for aspect dependence

Details Highly ionized stellar winds in Be stars - The evidence for aspect dependence Highly ionized stellar winds in Be stars - The evidence for aspect dependence

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...320..376g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 320, Sept. 1, 1987, p. 376-397.

Astronomy and Astrophysics

Astrophysics

66

B Stars, Early Stars, Ion Production Rates, Stellar Spectrophotometry, Stellar Winds, Ultraviolet Spectra, Line Spectra, Stellar Luminosity, Wind Velocity

Scientific paper

The authors present the results of an ultraviolet survey of stellar winds in 62 Be and 43 normal B stars covering spectral types B0.5 - B5 and luminosity classes V - III. They find that the wind absorption seen in the resonance lines of C IV, Si IV, and Si III in Be stars is often the result of blended absorption from multiple shortward-shifted discrete absorption components. There is evidence of a threshold in v sin i for the presence of strong and highly variable winds in Be stars. Wind absorption in the form of shortward-shifted discrete components is observed only for Be stars having v sin i ≥ 150 km s-1. The recent discovery that many, if not all, Be stars appear to be nonradial pulsators, and the observation that the pulsation characteristics of these stars change at v sin i = 150 km s-1 suggests that nonradial pulsation may be important in generating the Be phenomenon. The authors also present evidence that the high-velocity and highly ionized stellar wind observed in some, but not all, moderate to high v sin i Be stars is a function of latitude.

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