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@article{2210840, author = {Krtička, Jiří and Kubát, Jiří and Krtičková, Iva}, article_number = {March}, doi = {http://dx.doi.org/10.1051/0004-6361/202142502}, keywords = {X-rays: binaries; stars: winds; outflows; stars: mass-loss; stars: early-type; stars: massive; hydrodynamics}, language = {eng}, issn = {0004-6361}, journal = {Astronomy & Astrophysics}, title = {X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs}, url = {https://www.aanda.org/articles/aa/full_html/2022/03/aa42502-21/aa42502-21.html}, volume = {659}, year = {2022} }
TY - JOUR ID - 2210840 AU - Krtička, Jiří - Kubát, Jiří - Krtičková, Iva PY - 2022 TI - X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs JF - Astronomy & Astrophysics VL - 659 IS - March SP - 1-11 EP - 1-11 PB - EDP Sciences SN - 00046361 KW - X-rays: binaries KW - stars: winds KW - outflows KW - stars: mass-loss KW - stars: early-type KW - stars: massive KW - hydrodynamics UR - https://www.aanda.org/articles/aa/full_html/2022/03/aa42502-21/aa42502-21.html N2 - Wind-fed high-mass X-ray binaries are powered by accretion of the radiatively driven wind of the luminous component on the compact star. Accretion-generated X-rays alter the ionization state of the wind. Because higher ionization states drive the wind less effectively, X-ray ionization may brake acceleration of the wind. This causes a decrease in the wind terminal velocity and mass flux in the direction toward the X-ray source. Here we study the effect of X-ray ionization on the stellar wind of B supergiants. We determine the binary parameters for which the X-ray irradiation significantly influences the stellar wind. This can be conveniently studied in diagrams that plot the optical depth parameter versus the X-ray luminosity. For low optical depths or for high X-ray luminosities, X-ray ionization leads to a disruption in the wind aimed toward the X-ray source. Observational parameters of high-mass X-ray binaries with B-supergiant components appear outside the wind disruption zone. The X-ray feedback determines the resulting X-ray luminosity. We recognize two states with a different level of feedback. For low X-ray luminosities, ionization is weak, and the wind is not disrupted by X-rays and flows at large velocities, consequently the accretion rate is relatively low. On the other hand, for high X-ray luminosities, the X-ray ionization disrupts the flow braking the acceleration, the wind velocity is low, and the accretion rate becomes high. These effects determine the X-ray luminosity of individual binaries. Accounting for the X-ray feedback, estimated X-ray luminosities reasonably agree with observational values. We study the effect of small-scale wind inhomogeneities (clumping), showing that clumping weakens the effect of X-ray ionization by increasing recombination and the mass-loss rate. This effect is particularly important in the region of the so-called bistability jump. We show that ultraluminous X-ray binaries with LX less than or similar to 10(40) erg s(-1) may be powered by accretion of a B-supergiant wind on a massive black hole. ER -
KRTIČKA, Jiří, Jiří KUBÁT a Iva KRTIČKOVÁ. X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs. Online. \textit{Astronomy \&{} Astrophysics}. EDP Sciences, 2022, roč.~659, March, s.~1-11. ISSN~0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/202142502. [citováno 2024-04-24]
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