Wind Dynamics in SMC X-1. I. Hydrodynamic Simulation
Abstract
We present a three-dimensional hydrodynamic simulation of the disrupted stellar wind in the high-mass X-ray binary system SMC X-1. The three dominant processes that determine the geometry of the wind in high X-ray luminosity systems such as SMC X-1 are the X-ray suppression of the stellar wind from the X-ray irradiated face of the primary star, the focusing of the radiatively driven wind in the X-ray shadow by the effects of stellar rotation, and the rapid X-ray heating of gas in the vicinity of the X-ray source, including the X-ray illuminated surface of the primary star. The resulting distribution of circumstellar gas provides a successful explanation for the asymmetric, extended eclipse transitions and the intensity of the deep eclipse X-ray emission in SMC X-1, as well as a possible explanation for the X-ray dips seen near superior conjunction of the X-ray source in Cyg X-1.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- June 1995
- DOI:
- 10.1086/175748
- Bibcode:
- 1995ApJ...445..889B
- Keywords:
-
- Hydrodynamic Equations;
- Radiation Pressure;
- Stellar Envelopes;
- Stellar Winds;
- Three Dimensional Models;
- X Ray Binaries;
- Photoionization;
- Radiative Transfer;
- Stellar Luminosity;
- Stellar Mass Ejection;
- Stellar Rotation;
- Astrophysics;
- HYDRODYNAMICS;
- STARS: CIRCUMSTELLAR MATTER;
- STARS: INDIVIDUAL ALPHANUMERIC: SMC X-1;
- STARS: MASS LOSS;
- X-RAYS: STARS