Winds from rotating, magnetic, hot stars - Consequences for the rotational evolution of O and B stars

Details Winds from rotating, magnetic, hot stars - Consequences for the rotational evolution of O and B stars Winds from rotating, magnetic, hot stars - Consequences for the rotational evolution of O and B stars

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...256..141m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 256, no. 1, p. 141-147.

Astronomy and Astrophysics

Astrophysics

10

B Stars, Hot Stars, O Stars, Stellar Evolution, Stellar Magnetic Fields, Stellar Rotation, Magnetic Flux, Stellar Mass Ejection

Scientific paper

In an effort to obtain estimates of magnetic field strengths in hot stars, we have computed the evolution of rigidly rotating 15 and 30 solar mass stars, including the effects of magnetically coupled, line-driven mass loss as described by the model of Friend & MacGregor (1984). Using mean rotational velocities (i.e. v sin i values) derived from observations of main-sequence stars of these masses to specify the initial state, we followed the variations in time of the surface rotation rate due to internal structural changes and wind-related breaking. In each case the initial magnetic field strength was varied until the calculated rotational velocity at the onset of the blue supergiant phase was in reasonable agreement with the corresponding mean v sin i value derived from observations. For both evolutionary models, we find that the computed rotational velocity decrease in the presence of a magnetic field of even modest strength (less than about 100 G) exceeds the limits set by observations. The limitations of this study and its implications for both the magnetic fields and winds of hot stars are discussed.

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