The expanding envelope of Tau SCO (B0 V)

Details The expanding envelope of Tau SCO (B0 V) The expanding envelope of Tau SCO (B0 V)

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....66..417l&link_type=abstract

Astronomy and Astrophysics, vol. 66, no. 3, June 1978, p. 417-430.

Astronomy and Astrophysics

Astronomy

112

Absorption Spectra, Early Stars, Stellar Atmospheres, Stellar Envelopes, Stellar Mass Ejection, Ultraviolet Spectra, Line Spectra, Optical Thickness, Spaceborne Astronomy, Stellar Models, Stellar Spectra, Stellar Winds

Scientific paper

Results are reported for an analysis of the UV spectrum of Tau Sco as observed by Copernicus. It is found that the spectrum exhibits a number of resonance lines of C III, C IV, N III, N V, O VI, Si IV, and P V, all of which have extended violet absorption wings that reach several different velocities. The UV lines of Tau Sco are compared with those of Zeta Pup, the line profiles are studied by a comparison with predicted profiles, and the optical depth of the lines is derived as a function of velocity in the envelope by means of line fitting. The velocity-height relation is examined, the mass-loss rate is derived, and the ionization equilibrium in the envelope is investigated. The data are then evaluated in light of three proposed mass-loss mechanisms. The mass-loss rate is estimated to be about 7 billionths of a solar mass per year, and the observed rapid acceleration of the stellar wind is attributed to radiation pressure in the envelope. It is shown that an imperfect-flow model for the stellar wind gives qualitative agreement with the observations.

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