X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00556343" target="_blank" >RIV/67985815:_____/22:00556343 - isvavai.cz</a>
Alternative codes found
RIV/00216224:14310/22:00126397
Result on the web
<a href="https://doi.org/10.1051/0004-6361/202142502" target="_blank" >https://doi.org/10.1051/0004-6361/202142502</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/202142502" target="_blank" >10.1051/0004-6361/202142502</a>
Alternative languages
Result language
angličtina
Original language name
X-ray irradiation of the stellar wind in HMXBs with B supergiants: Implications for ULXs
Original language description
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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/LM2018140" target="_blank" >LM2018140: e-Infrastructure CZ</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2022
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astronomy & Astrophysics
ISSN
0004-6361
e-ISSN
1432-0746
Volume of the periodical
659
Issue of the periodical within the volume
March
Country of publishing house
FR - FRANCE
Number of pages
11
Pages from-to
A117
UT code for WoS article
000769069100007
EID of the result in the Scopus database
2-s2.0-85126831981