Rates of mass loss from O-stars

Details Rates of mass loss from O-stars Rates of mass loss from O-stars

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....93..163c&link_type=abstract

Astronomy and Astrophysics, vol. 93, no. 1-2, Jan. 1981, p. 163-170. Research supported by the Consiglio Nazionale delle Ricerc

Astronomy and Astrophysics

Astrophysics

27

O Stars, Stellar Mass Ejection, Stellar Radiation, Early Stars, Radiation Pressure, Stellar Luminosity, Stellar Mass, Stellar Temperature, Stellar Winds

Scientific paper

The mass-loss rates, luminosities, effective temperatures, and masses of O, O1, and Of stars are discussed to empirically derive the law that controls the rate of mass loss from these objects. We find a dependence of mass-loss rate on basic stellar parameters that substantially differs from the one predicted by the line radiation pressure theory. Single WR stars seem also to obey the same relationship.
The physical implications of this result are brought out at some extent by generalizing the empirical law for the rate of mass loss.
We conclude emphasizing that the winds may be driven by the same mechanism acting in all early type stars. This analysis might point out that the radiation pressure mechanism is not the cause of the flow, which is perhaps due to non thermal energy storage in the stellar interiors, but only modulates the velocity field at large distances.

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