Modeling of hydrodynamic processes within high-mass X-ray binaries
| Authors | |
|---|---|
| Year of publication | 2019 |
| Type | Article in Proceedings |
| Conference | Symposium S346 (High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects) |
| MU Faculty or unit | |
| Citation | |
| Web | https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/modeling-of-hydrodynamic-processes-within-highmass-xray-binaries/E1B9FB24CB1909F5CAF3FEAEC4289AC2 |
| Doi | http://dx.doi.org/10.1017/S1743921319000024 |
| Keywords | massive stars; evolution; mass-loss; accretion; supernovae |
| Description | High-mass X-ray binaries belong to the brightest objects in the X-ray sky. They usually consist of a massive O or B star or a blue supergiant while the compact X-ray emitting component is a neutron star (NS) or a black hole. Intensive matter accretion onto the compact object can take place through different mechanisms: wind accretion, Roche-lobe overflow, or circumstellar disk. In our multi-dimensional models we perform numerical simulations of the accretion of matter onto a compact companion in case of Be/X-ray binaries. Using Bondi-Hoyle-Littleton approximation, we estimate the NS accretion rate. We determine the Be/X-ray binary disk hydrodynamic structure and compare its deviation from isolated Be stars’ disk. From the rate and morphology of the accretion flow and the X-ray luminosity we improve the estimate of the disk mass-loss rate. We also study the behavior of a binary system undergoing a supernova explosion, assuming a blue supergiant progenitor with an aspherical circumstellar environment. |
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