Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-25T17:37:59.254Z Has data issue: false hasContentIssue false
  • English
  • Français

Modeling of hydrodynamic processes within high-mass X-ray binaries

Published online by Cambridge University Press:  30 December 2019

Petr Kurfürst  and
Jiří Krtička
Petr Kurfürst
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, CZ-611 37 Brno, Czech Republic emails: [email protected], [email protected] Institute of Theoretical Physics, Charles University, V Holešovičkách 2, 180 00 Praha 8, Czech Republic email: [email protected]
Jiří Krtička
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Kotlářská 2, CZ-611 37 Brno, Czech Republic emails: [email protected], [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Keywords

massive starsevolutionmass-lossaccretionsupernovae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 197 - 201
Copyright
© International Astronomical Union 2019 

References

Chevalier, R. A. 1989, ApJ, 258, 790C 10.1086/160126CrossRefGoogle Scholar
Krtička, J., Kurfürst, P., & Krtičková, I. 2015, A&A, 573, 20K Google Scholar
Kurfürst, P., Feldmeier, A., & Krtička, J. 2014, A&A, 569, 23K Google Scholar
Kurfürst, P., Feldmeier, A. & Krtička, J. 2018, A&A, 613, A75 Google Scholar
Lee, U., Osaki, Y., & Saio, H. 1991, MNRAS, 250, 432L 10.1093/mnras/250.2.432CrossRefGoogle Scholar
Morozova, V., Piro, A. L., & Renzo, M. 2015, ApJ, 814, 63 10.1088/0004-637X/814/1/63CrossRefGoogle Scholar
Okazaki, A. T., & Negueruela, I. 2001, A&A, 377, 161 Google Scholar
Reig, P. 2011, Ap&SS, 332, 1R Google Scholar
Rivinius, T., Carciofi, A. C., & Martayan, C. 2013, A&ARv, 21, 69R Google Scholar