The rate of mass loss and variations in the wind from the Be star Delta Centauri

Details The rate of mass loss and variations in the wind from the Be star Delta Centauri The rate of mass loss and variations in the wind from the Be star Delta Centauri

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...242.1077s&link_type=abstract

Astrophysical Journal, Part 1, vol. 242, Dec. 15, 1980, p. 1077-1082.

Astronomy and Astrophysics

Astrophysics

10

B Stars, Stellar Mass Ejection, Stellar Spectra, Stellar Winds, Ultraviolet Spectra, Centaurus Constellation, Oao 3, Photosphere, Stellar Luminosity

Scientific paper

Copernicus ultraviolet scans of the Be star δ Centauri, obtained in 1976 and 1979, show a significant variation in the Si III λ1206 profile, the strong asymmetry that was present in 1976 having disappeared by 1979. The Si IV λ140O doublet was also asymmetric in 1976, but was not observed in 1979. A quantitative fit of the line shapes to theoretical wind profiles shows that the mass-loss rate in 1976 was 2.0 × 1--10 yr-1 and that the rate of mass loss in S III was at least one order of magnitude less in 1979. It is not possible to determine whether the variation represented an overall change in the mass-loss rate or whether it was due to a change in the ionization balance. The profile-fitting procedure resulted in the adoption of assumed underlying photospheric Si III and Si IV profiles, and the equivalent widths measured from these profiles are most consistent with teff between 30,000 and 35,000 K, somewhat hotter than implied by the spectral classification normally assigned to this star. The ultraviolet photospheric line widths, coupled with published theoretical analyses of rotational gravitational darkening, imply an intrinsic equatorial velocity of about 310 km s-1 and an angle of inclination of the rotational axis to the line of sight of i ≤ 440.

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