Wind models for zeta Orionis.
Abstract
Several models of the winds of O stars have been proposed to explain the unexpected presence of ions with a high ionization potential, such as N(+4) and O(+5). Olson (1978) has explained the presence of these ions by showing that in a thin corona, at the base of a cool wind, these ions can be produced by the Auger photoionization process, where a single X-ray photon will eject two electrons. Another possibility is that the winds are only at a slightly elevated temperature (40,000 to 60,000 K) and that photoionization in an optically thick wind generates the unexpected ions. The purpose of the present analysis is to test the capability of some existing wind models to fit the observations of Zeta Orionis. Rough model calculations indicate that the corona-cool wind model fits the observations better than the 'warm' or 'tepid' wind models.
- Publication:
-
Mass Loss and Evolution of O-Type Stars
- Pub Date:
- 1979
- Bibcode:
- 1979IAUS...83..257O
- Keywords:
-
- O Stars;
- Stellar Models;
- Stellar Winds;
- Ion Density (Concentration);
- Line Spectra;
- Stellar Mass Ejection;
- Ultraviolet Spectra;
- Astrophysics;
- Mass Loss:Models;
- Stellar Winds:Models