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Fossil magnetic fields and rotation of early-type stars

Published online by Cambridge University Press:  26 May 2016

A.E. Dudorov
A.E. Dudorov*
Affiliation:
Chelyabinsk State University, Russia

Extract

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Observational data of the last 10 years allow two main conclusions:

a) Main sequence stars can be separated in two classes: - magnetic (Bp) stars with surface strengths of a dipole or quadrupole magnetic field of Bs ≈ n · (102 − 103) G, n = 2,3,4…7, and - normal main sequence stars (F-O) with magnetic fields Bs ≈ 1 − 100 G (< 300 G);

b) Typical star formation takes place in interstellar molecular clouds with magnetic field strengths B ≈ 10-5 G (See Dudorov 1990).

Type
2. Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 184 - 185
Copyright
Copyright © Kluwer 1994 

References

Dudurov, A.E. 1977a, in Early Stages of Stellar Evolution, ed. Kolesnik, I.G., Kiev: Naukova Dumka, 56 (In Russian).Google Scholar
Dudorov, A.E. 1990, Magnetic Fields of Interstellar Clouds (Moscow: VINITI), 158 (In Russian).Google Scholar
Dudorov, A.E. and Sazonov, Yu.V. 1981, Nauchnye Informatsii Astronomicheskogo Soveta AN SSSR, 49, 114 (In Russian).Google Scholar
Dudorov, A.E. and Sazonov, Yu.V. 1987, ibid, 63, 68.Google Scholar