X-ray irradiation of the stellar wind in HMXBs with B
supergiants: Implications for ULXs

J 2022

X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs

KRTIČKA, Jiří; Jiří KUBÁT a Iva KRTIČKOVÁ

Základní údaje

Originální název

X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs

Autoři

KRTIČKA, Jiří; Jiří KUBÁT a Iva KRTIČKOVÁ

Vydání

Astronomy & Astrophysics, EDP Sciences, 2022, 0004-6361

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

URL

Impakt faktor

Impact factor: 6.500

Označené pro přenos do RIV

Ano

Kód RIV

RIV/00216224:14310/22:00126397

Organizační jednotka

Přírodovědecká fakulta

Klíčová slova anglicky

X-rays: binaries; stars: winds; outflows; stars: mass-loss; stars: early-type; stars: massive; hydrodynamics

Štítky

14312040, rivok

Příznaky

Mezinárodní význam, Recenzováno

Změněno: 9. 8. 2022 14:37, Mgr. Marie Novosadová Šípková, DiS.

Anotace

V originále

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.

Návaznosti

LM2018140, projekt VaV

Název: e-Infrastruktura CZ (Akronym: e-INFRA CZ)

Investor: Ministerstvo školství, mládeže a tělovýchovy ČR, e-Infrastruktura CZ

Citovat

KRTIČKA, Jiří; Jiří KUBÁT a Iva KRTIČKOVÁ. X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs. Astronomy & Astrophysics. EDP Sciences, 2022, roč. 659, March, s. 1-11. ISSN 0004-6361. Dostupné z: https://doi.org/10.1051/0004-6361/202142502.

@article{2210840,
   author = {Krtička, Jiří and Kubát, Jiří and Krtičková, Iva},
   article_number = {March},
   doi = {https://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. \textit{Astronomy \&{} Astrophysics}. EDP Sciences, 2022, roč.~659, March, s.~1-11. ISSN~0004-6361. Dostupné z: https://doi.org/10.1051/0004-6361/202142502.

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