Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...528..965a&link_type=abstract
The Astrophysical Journal, Volume 528, Issue 2, pp. 965-971.
Astronomy and Astrophysics
Astronomy
20
Magnetohydrodynamics: Mhd, Stars: Individual: Constellation Name: &Alpha, Orionis, Stars: Winds, Outflows, Stars: Supergiants, Waves
Scientific paper
We present the results of magnetohydrodynamic (MHD) modeling of winds from luminous late-type stars using a 2.5-dimensional, nonlinear MHD computer code. We assume that the wind is generated within an initially hydrostatic atmosphere and is driven by torsional Alfvén waves generated at the stellar surface. Two cases of atmospheric topology are considered: case I has longitudinally uniform density distribution and isotropic radial magnetic field over the stellar surface, and case II has an isotropic, radial magnetic field with a transverse density gradient, which we refer to as an ``atmospheric hole.'' We use the same set of boundary conditions for both models.The calculations are designed to model a cool luminous star, for which we assume an initial hydrostatic pressure scale height of 0.072 R*, an Alfvén wave speed of 92 km s-1 at the surface, and a wave period of 76 days, which roughly corresponds with the convective turnover time. For case I the calculations produce a wind with terminal velocity of ~22 km s-1 and a mass loss rate comparable to the expected value of 10-6 Msolar yr-1. For case II we predict a two-component wind: a fast (25 km s-1) and relatively dense wind outside of the atmospheric hole and a slow (15 km s-1), rarefied wind inside of the hole.
Airapetian Vladimir S.
Carpenter Ken
Davila Javier
Ofman Leon
Robinson Richard D.
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