Evidence for Optically Thick, Eddington-limited Winds Driven by Supercritical Accretion

Zhou, Yu; Feng, Hua; Ho, Luis C.; Yao, Yuhan

doi:10.3847/1538-4357/aaf724

Cited by 16 publications

(21 citation statements)

References 94 publications

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“…For the wind speed we consider the escape velocity of the gravitational attraction of the central black hole. In the calculations we adoptė = 1, which is consistent with what was found by Zhou et al (2019).…”

Section: Disk and Windsupporting

confidence: 83%

Model for Population III microquasars

Checa

Romero

2019

A&A

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Context. Current simulations indicate that the first stars were formed predominantly in binary systems. Studying the contribution of the first accreting binary systems to the reionization and heating of the intergalactic medium requires formulating a concrete model for Population III microquasars. Aims. We aim at constructing a complete model for microquasars with a Population III donor star. Methods. We considered that the mass loss of the star is exclusively caused by the spill of matter through the Roche lobe toward the black hole. We calculated the spectral energy distribution of the radiation produced by the accretion disk, the radiation-pressure-driven wind, and the relativistic particles in the jets, within the framework of a lepto-hadronic model. In addition, we estimated the effect on the reionization by the first microquasars. Results. We determine that Population III microquasars are powerful sources of ultraviolet radiation produced by the winds of their super-critical disks, and that they generate a broadband nonthermal emission in jets. Conclusions. Our results indicate that microquasars in the early Universe could have been important for the reionization and heating of the intergalactic medium.

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Section: Disk and Windsupporting

confidence: 83%

Model for Population III microquasars

Checa

Romero

2019

A&A

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“…3). When the accretion disc is edge-on (low state) we only see the super-soft component from the disc and disc wind that create a photosphere (Zhou et al 2019). Thus, during its low state M51 ULX-7 is an analog to the ultraluminous super-soft X-ray sources like NGC 55 ULX (Pinto et al 2017).…”

Section: Discussionmentioning

confidence: 99%

M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

Vasilopoulos

Lander

Koliopanos

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the current work we explore the applicability of standard theoretical models of accretion to the observed properties of M51 ULX-7. The spin-up rate and observed X-ray luminosity are evidence of a neutron star with a surface magnetic field of 2 − 7 × 10 13 G, rotating near equilibrium. Analysis of the X-ray light-curve of the system (Swift/XRT data) reveals the presence of a ∼39 d super-orbital period. We argue that the super-orbital periodicity is due to disc precession, and that material is accreted onto the neutron star at a constant rate throughout it. Moreover, by attributing this modulation to the free precession of the neutron star we estimate a surface magnetic field strength of 3 − 4 × 10 13 G. The agreement of these two independent estimates provide strong constraints on the surface polar magnetic field strength of the neutron star.

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“…Ohsuga & Mineshige 2011;Takeuchi et al 2013), which may themselves be optically thick (and therefore contribute blackbody-like emission) and shroud the outer accretion flow (e.g. King & Pounds 2003;Urquhart & Soria 2016;Zhou et al 2019).…”

Section: The Non-magnetic Accretor Modelmentioning

confidence: 99%

The unusual broad-band X-ray spectral variability of NGC 1313 X-1 seen with XMM–Newton, Chandra, and NuSTAR

Walton

Pinto

Nowak

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present results from the major coordinated X-ray observing programme on the ULX NGC 1313 X-1 performed in 2017, combining XMM–Newton, Chandra, and NuSTAR, focusing on the evolution of the broad-band (∼0.3–30.0 keV) continuum emission. Clear and unusual spectral variability is observed, but this is markedly suppressed above ∼10–15 keV, qualitatively similar to the ULX Holmberg IX X-1. We model the multi-epoch data with two-component accretion disc models designed to approximate super-Eddington accretion, allowing for both a black hole and a neutron star accretor. With regards to the hotter disc component, the data trace out two distinct tracks in the luminosity–temperature plane, with larger emitting radii and lower temperatures seen at higher observed fluxes. Despite this apparent anticorrelation, each of these tracks individually shows a positive luminosity–temperature relation. Both are broadly consistent with L ∝ T4, as expected for blackbody emission with a constant area, and also with L ∝ T2, as may be expected for an advection-dominated disc around a black hole. We consider a variety of possibilities for this unusual behaviour. Scenarios in which the innermost flow is suddenly blocked from view by outer regions of the super-Eddington disc/wind can explain the luminosity–temperature behaviour, but are difficult to reconcile with the lack of strong variability at higher energies, assuming this emission arises from the most compact regions. Instead, we may be seeing evidence for further radial stratification of the accretion flow than is included in the simple models considered, with a combination of winds and advection resulting in the suppressed high-energy variability.

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Evidence for Optically Thick, Eddington-limited Winds Driven by Supercritical Accretion

Cited by 16 publications

References 94 publications

Model for Population III microquasars

Model for Population III microquasars

M51 ULX-7: superorbital periodicity and constraints on the neutron star magnetic field

The unusual broad-band X-ray spectral variability of NGC 1313 X-1 seen with XMM–Newton, Chandra, and NuSTAR

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