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The Effects of a Weak Magnetic Field in the Line Profiles of A-type Supergiant Winds

Published online by Cambridge University Press:  12 April 2016

E. Verdugo ,
A. de Castro Gómez ,
C. Ferro-Fontán  and
A. Talavera
E. Verdugo
Affiliation:
ISO Data Centre, VILSPA P.O.Box 50727, 28080 Madrid, Spain
A. de Castro Gómez
Affiliation:
Instituto de Astronomía y Geodesia(CSIC-UCM), Fac. cc. Matemáticas, Universidad Complutenses/n, E-28040-Madrid, Spain
C. Ferro-Fontán
Affiliation:
Instituto de Fíca del Plasma, Universidad de Buenos Aires, Consejo Nacional de Investigaciones Científicas y Técnicas and Deparatamento de Física, Ciudad Universitaria, 1428 Buenos Aires, Argentina
A. Talavera
Affiliation:
XMM Newton Obs., VILSPA P.O.Box 50727, 28080 Madrid, Spain

Extract

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Solutions for the stellar winds of hot luminous stars are obtained by solving the magnetohydrodynamic (MHD) equations, combined with the theory of radiation-driven winds. The formalism is basically the same as developed by Rotstein & Giménez de Castro (1996). We have considered the interaction of radiation pressure with an open magnetic field . The magnetic field lines are pushed by the intense radiation field and adopt a purely radial configuration:

and the polar magnetic flux at the photosphere:

Rotstein & Giménez de Castro (1996) assume all the lines contributing to the radiation pressure are optically thick (α = 1) in order to decouple the MHD equations. Here the model has been improved to adopt a value of α = 0.6 which is a better approach for A-supergiants.

Type
Part 5. Mass Loss in Pulsating Stars
Information
International Astronomical Union Colloquium , Volume 185: Radial and Nonradial Pulsations as Probes of Stellar Physics , 2002 , pp. 574 - 575
Copyright
Copyright © Astronomical Society of the Pacific 2002

References

Rotstein, N., Giménez, de Castro, C.G. 1996, ApJ, 464, 859 Google Scholar