Volume 405, Number 1, July I 2003
|Page(s)||165 - 174|
|Section||Interstellar and circumstellar matter|
|Published online||16 June 2003|
Ionization structure in the winds of B[e] supergiants
I. Ionization equilibrium calculations in a H plus He wind
Astronomical Institute, University of Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands e-mail: email@example.com
Corresponding author: M. Kraus, firstname.lastname@example.org
Accepted: 3 April 2003
The non-spherically symmetric winds of B[e] supergiants are investigated. An empirical density distribution is chosen that accounts for the density concentrations and ratios derived from observations, and our model winds are assumed to contain only hydrogen and helium. We first calculate the approximate ionization radii for H and He and compare the results with the ionization fractions calculated from the more accurate ionization balance equations. We find that winds with a r-2 density distribution turn out to reach a constant ionization fraction as long as the wind density is low, i.e. in polar direction. For the high density equatorial regions, however, we find that the winds become neutral just above the stellar surface of the hot and massive B[e] supergiants forming a disk-like neutral region. In such a disk molecules and dust can form even very near the hot central star.
Key words: supergiants / stars: mass-loss / stars: winds, outflows / HII regions
© ESO, 2003
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