Wind-powered Ultraluminous X-ray Sources

Wiktorowicz, Grzegorz; Lasota, Jean–Pierre; Belczyński, Krzysztof; Lu, Youjun; Liu, Jifeng; Iłkiewicz, Krystian

doi:10.3847/1538-4357/ac0cf7

Cited by 13 publications

(5 citation statements)

References 85 publications

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“…We make the SED ULX models at each metallicity available as part of this work (Section 5.4), noting they represent only the accretion flow and therefore do not account for any emission related to the putative donor star. We have implemented the SED ULX without selecting a unique donor star, in part because the distribution of such sources for ULXs, though the subject of intense study, is still not well constrained theoretically or observationally (e.g., Liu et al 2004;Copperwheat et al 2005;Motch et al 2011;Tao et al 2011;Grisé et al 2012;Soria et al 2012;Gladstone et al 2013;Heida et al 2014Heida et al , 2016Heida et al , 2019aHeida et al , 2019bWiktorowicz et al 2017Wiktorowicz et al , 2021Lau et al 2019). Identifying unique optical, UV, or IR counterparts at the extragalactic distances to most ULXs remains challenging.…”

Section: Parameterization Of Sed Shapementioning

confidence: 99%

Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Garofali,

Basu-Zych,

Johnson

et al. 2023

ApJ

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We present a methodology for modeling the joint ionizing impact due to a “simple X-ray population” (SXP) and its corresponding simple stellar population (SSP), where “simple” refers to a single age and metallicity population. We construct composite spectral energy distributions (SEDs) including contributions from ultraluminous X-ray sources and stars, with physically meaningful and consistent consideration of the relative contributions of each component as a function of instantaneous burst age and stellar metallicity. These composite SEDs are used as input for photoionization modeling with Cloudy, from which we produce a grid for the time- and metallicity-dependent nebular emission from these composite populations. We make the results from the photoionization simulations publicly available. We find that the addition of the SXP prolongs the high-energy ionizing output from the population—and correspondingly increases the intensity of nebular lines such as He ii λ1640,4686, [Ne v] λ3426,14.3 μm, and [O iv] 25.9 μm by factors of at least two relative to models without an SXP spectral component. This effect is most pronounced for instantaneous bursts of star formation on timescales >10 Myr and at low metallicities (∼0.1 Z ⊙), due to the imposed time- and metallicity-dependent behavior of the SXP relative to the SSP. We propose nebular emission line diagnostics accessible with JWST suitable for inferring the presence of a composite SXP + SSP, and we discuss how the ionization signatures compare to models for sources such as intermediate-mass black holes.

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Section: Parameterization Of Sed Shapementioning

confidence: 99%

Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Garofali,

Basu-Zych,

Johnson

et al. 2023

ApJ

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“…Typical ULXs have X-ray luminosities in excess of 10 39 erg s −1 (Swartz et al 2004;Walton et al 2011). Although the ULXs are believed to be powered mostly by Roche lobe overflow (Karino 2018;El Mellah et al 2019), the wind accretion remains a viable option at least for some of these sources (Miller et al 2014;Wiktorowicz et al 2021).…”

Section: Implications For Ulxsmentioning

confidence: 99%

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

Krtička

Kubát

Krtičková

2022

A&A

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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 ≲ 1040 erg s−1 may be powered by accretion of a B-supergiant wind on a massive black hole.

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“…Up to the accepted normalization, the total number of ULX in our calculations (see Fig. In a recent paper by Wiktorowicz et al (2021), accretion from the stellar wind was considered. In this paper, the interpretation of Bondi-Hoyle-Littleton accretion for elliptical orbits is, however, significantly different from that in our study.…”

Section: Comparison To Other Studiesmentioning

confidence: 99%

Populations of ultraluminous X-ray sources in galaxies: origin and evolution

Kuranov,

Postnov,

Yungelson

2021

Preprint

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Employing hybrid population synthesis, a model of the population of ultraluminous X-ray sources (ULX) in the binary systems with a black hole (BH) accretors is computed.It is compared to the model of the population of ULX with magnetized neutron stars (NS) that can be observed as pulsating ULX (Kuranov et al. 2020). A model of formation of BH is considered, in which their mass is determined by the mass of stellar CO core immediately before the collapse (M CO ), as well as "delayed" and "rapid" collapse models (Fryer et al. 2012). Possible transiency of ULX due to accretion disks instability is taken into accountThe parameters and evolution of ULX are computed for the galaxies with constant star formation rate (SFR) and for the ones formed by an instantaneous star formation burst.The maximum number of ULX with BH (∼ 10) is reached in the galaxies with stationary SF R = 10M /yr in ∼ 1 Gyr after beginning of star formation. ULX which are observed after the end of star formation, are binaries, in which BH and/or NS formed before the completion of star formation, while long-living donors with the mass ∼ M continue RLOF or even fill their Roche lobes later. In several Gyr after completion of star formation the number of ULX in the galaxies with mass M G = 10 10 M becomes less than 1 per 10 galaxies, most of them are ULX with NS. In ULX with NS, regardless of the adopted SFR model, dominate persistent sources with the donor overflowing Roche lobe. The number of transient sources is by more than an order of magnitude lower. Wind-accreting ULX are by an order of magnitude more rare than the sources with accretion via RLOF.

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Wind-powered Ultraluminous X-ray Sources

Cited by 13 publications

References 85 publications

Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

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

Populations of ultraluminous X-ray sources in galaxies: origin and evolution

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