X-Ray Emission in Wind Instability Simulations
Abstract
We estimate X-ray emission by shock-heated regions in hot star winds, using temperature and density profiles calculated by time-dependent dynamical models; the shocks result from the instability of the line scattering force that drives the wind. For main sequence late O and early B stars, the model X-ray flux is generally well below the observed flux, though the shape of the model spectrum is approximately consistent with observations. For the early O supergiantζ Pup, the model spectral shape again agrees with observation; the total flux predicted by models is well above the observed flux, though significant uncertainties remain.
- Publication:
-
Astrophysics and Space Science
- Pub Date:
- November 1994
- DOI:
- 10.1007/BF01091172
- Bibcode:
- 1994Ap&SS.221..427C
- Keywords:
-
- B Stars;
- Computational Astrophysics;
- Main Sequence Stars;
- O Stars;
- Shock Waves;
- Stellar Physics;
- Stellar Winds;
- Temperature Profiles;
- X Ray Astronomy;
- X Rays;
- Computerized Simulation;
- Density Distribution;
- Line Spectra;
- Shock Heating;
- Spectrum Analysis;
- Stellar Models;
- Time Dependence;
- Astrophysics;
- X-rays;
- Winds;
- Hot Stars