Magnetohydrodynamic flows in Be stars - Variable energy flux and heat input distribution

Details Magnetohydrodynamic flows in Be stars - Variable energy flux and heat input distribution Magnetohydrodynamic flows in Be stars - Variable energy flux and heat input distribution

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...411..342i&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 411, no. 1, p. 342-350.

Other

5

B Stars, Magnetic Field Configurations, Magnetohydrodynamic Flow, Stellar Magnetic Fields, Stellar Mass Ejection, Stellar Rotation, Emission Spectra, Gravitational Fields, Line Spectra, Stellar Temperature, Stellar Winds

Scientific paper

We have worked out the equations of conservation of mass, momentum, and energy for the case of steady outflows in a rotating magnetic field, introducing a polytropic-type relation between pressure and density, with a variable index. We have determined sets of parameters that bring up the critical points that are needed to select a unique solution for the wind, and finally we have chosen those sets that can reproduce better the conditions observed in Be stars. Each solution depends on the choice of six nondimensional parameters which are related to the fluxes of energy at the base of the wind and at infinity, to the gravitational field, to the effective temperature of the star, to rotation, and to the magnetic field. The corotation induced by the magnetic field increases the centrifugal force and accelerates the wind. The choice of a particular functional form for the polytropic index allows the formation of a heating-accelerating region where the temperature increases with expansion and where larger temperatures and larger expansion values are obtained for strongly magnetized flows. Outside this region, temperature and rotation decay and the magnetic field yield two solutions of different asymptotic behavior: in one solution the velocity accelerates and in the other the velocity decelerates until they reach constant values.

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