Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mlao.conf...45c&link_type=abstract
Mass Loss from Astronomical Objects, Proceedings of a Rutherford Appleton Laboratory (RAL) Workshop on Astronomy and Astrophysic
Astronomy and Astrophysics
Astronomy
1
Black Holes (Astronomy), Gravitation, Kinetic Energy, Line Spectra, Stellar Luminosity, Stellar Winds, Wolf-Rayet Stars, B Stars, Cygnus Constellation, Early Stars, Giant Stars, Hot Stars, Ionizing Radiation, Losses, Morphology, Weight (Mass), Wind Velocity
Scientific paper
Stellar winds are observed in hot and luminous stars of all types. The evidence for the winds comes from observations of P Cygni profiles of resonance lines of highly ionized common species, from emission lines of highly excited ions, and from free-free radiation from the electrons in the outflowing material. Stellar winds have as their dominant origin the radiation pressure in the ultraviolet lines coupling momentum to the wind as a whole. It was found that for the most luminous OB stars, in which the winds can readily be detected, the mass loss rate is proportional to the luminosity, L, to a power alpha, where alpha is of the order of 1.7. This relation carries over four orders of magnitude in the mass loss rates. This relation also continues to the lower luminosity giant and main sequence B type stars. By contrast, the mass loss rates for the enigmatic Wolf-Rayet (W-R) stars, which have among themselves vastly different spectra, luminosities, and masses are similar.
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