Testing slim-disk models on the thermal spectra of LMC X-3

Straub, O.; Bursa, Michal; Sądowski, Aleksander; Steiner, James F.; Abramowicz, Marek A.; Kluźniak, W.; McClintock, Jeffrey E.; Narayan, Ramesh; Remillard, Ronald A.

doi:10.1051/0004-6361/201117385

Cited by 62 publications

(64 citation statements)

References 31 publications

(49 reference statements)

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“…The classical soft-state spectrum of the X-ray binary LMC X-3 in dominated by a ∼ 0.5kev. This result agrees with Straub et al (2011). Davis et al (2006), have plotted the spectrum of LMC X-3 for i = 60…”

Section: Resultssupporting

confidence: 87%

Radiation spectrum of a magnetized supercritical accretion disc with thermal conduction

Ghasemnezhad

Khajavi

Abbassi

2013

Astrophys Space Sci

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we examine the effect of thermal conduction on the observational properties of a super critical hot magnetized flow. We obtained self-similar solution of a magnetized disc when the thermal conduction plays an important role. Follow of our first paper (Ghasemnezhad et al. 2012 (hereafter GKA12)) we have extended our solution on the observational appearance of the disc to show how physical condition such as thermal conduction, viscosity, and advection will change the observed luminosity of the disc, Continuous spectra and surface temperature of such discs was plotted. We apply the present model to black-hole X-ray binary LMC X-3 and narrow-line seyfert 1 galaxies, which are supposed to be under critical accretion rate. Our results show clearly that the surface temperature is strongly depends on the thermal conduction, the magnetic field and advection parameter. However we see that thermal conduction acts to oppose the temperature gradient as we expect and observed luminosity of the disc will reduce when thermal conduction is high. We have shown that in this model the spectra of critical accretion flows strongly depends on the inclination angle.

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Section: Resultssupporting

confidence: 87%

Radiation spectrum of a magnetized supercritical accretion disc with thermal conduction

Ghasemnezhad

Khajavi

Abbassi

2013

Astrophys Space Sci

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“…Studies show that α = 0.1 is consistent with data from cataclysmic variables (e.g., King et al 2007), but inconsistent with data from X-ray binaries at moderate luminosities (e.g., Done & Davis 2008;Straub et al 2011). For a given luminosity and spin parameter a lower alpha value implies a higher ratio of absorption opacity to scattering opacity, which in turn implicates a higher optical depth, and thus a smaller colour correction factor.…”

Section: Effect Of Viscositymentioning

confidence: 74%

The effect of advection at luminosities close to Eddington: The ULX in M 31

Straub

Done

Middleton

2013

A&A

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The transient, ultra-luminous X-ray source CXOM31 J004253.1+411422 in the Andromeda galaxy is most likely a 10 solar mass black hole, with super-Eddington luminosity at its peak. The XMM-Newton spectra taken during the decline then trace luminosities of 0.86−0.27 L Edd . These spectra are all dominated by a hot disc component, which roughly follows a constant inner radius track in luminosity and temperature as the source declines. At the highest luminosity the disc structure should change due to advection of radiation through the disc. This advected flux can be partly released at lower radii thus modifying the spectral shape. To study the effect of advection at luminosities close to Eddington we employ a fully relativistic slim disc model, SLIMBH, that includes advective cooling and full radiative transfer through the photosphere based on tlusty. The model also incorporates relativistic photon raytracing from the proper location of the disc photosphere rather than the mid-plane as the slim disc is no longer geometrically thin. We find that these new models differ only slightly from the non-advective (standard) BHSPEC models even at the highest luminosities considered here. While both discs can fit the highest luminosity data, neither is a very good fit to the lower luminosities. This could indicate a missing physical process that acts in low luminosity discs and subsides as the disc luminosity approaches the Eddington limit.

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“…Indeed, the p-free disk approximation of an advectiondominated disk was sufficient to reproduce most of the BD ULX and the resampled BHB spectra. However, accretion disks are only thought to become sufficiently radiation pressure dominated to enter the slim-disk regime abovel 0.3 Steiner et al 2010;Straub et al 2011), whereas the BHB spectra appear to be broadened at values as low asl 0.1. We note that spectral shape is not the only difference between thin and slim disks, and a further test of the nature of these accretion disks could come from the luminosity-temperature relation.…”

Section: Discussionmentioning

confidence: 99%

Crossing the Eddington Limit: Examining Disk Spectra at High Accretion Rates

Sutton

Swartz

Roberts

et al. 2017

ApJ

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The faintest ultraluminous X-ray sources (ULXs), those with 0.3-10 keV luminosities 1 < L X /10 39 < 3 erg s −1 , tend to have X-ray spectra that are disk-like but broader than expected for thin accretion disks. These 'broadened disk' spectra are thought to indicate near-or mildly super-Eddington accretion onto stellar remnant black holes. Here we report that a sample of bright thermal-dominant black hole binaries, which have Eddington ratios constrained to moderate values, also show broadened disk spectra in the 0.3-10 keV band at an order of magnitude lower luminosities. This broadening would be missed in studies that only look above ∼ 2 keV. While this may suggest that broadened disk ULXs could be powered by accretion onto massive stellar remnant black holes with close to maximal spin, we argue in favor of a scenario where they are at close to the Eddington luminosity, such that radiation pressure would be expected to result in geometrically slim, advective accretion disks. However, this implies that an additional physical mechanism is required to produce the observed broad spectra at low Eddington ratios. −0.005 0.934 +0.006 −0.010 −1 ± 1 < 7 × 10 −4 47 (759.0/562) Swift-2 0.48 +0.02 −0.01 0.92 +0.02 −0.01 1.1 +0.6 −0.9 < 0.1 44 602.9/517 Resampled BHBs GX 339−4 XMM-1 1.0 ± 0.1 0.90 ± 0.02 3.6 ± 0.4 1.8 +0.7 −0.5 41 579.3/557 XMM-2 0.80 +0.08 −0.09 0.85 ± 0.02 2.6 +0.3 −0.4 0.8 +0.5 −0.3 44 561.6/564 LMC X-3 XMM-1 0.5 ± 0.1 1.37 +0.04 −0.03 4.6 +0.4 −0.5 6 ± 2 42 480.1/500 Swift-1 < 9 × 10 −3 1.164 +0.017 −0.009 2.2 +0.2 −0.1 0.50 +0.06 −0.04 43 435.5/391 XMM-2 [0] 1.16 +0.02 −0.03 2.5 +0.2 −0.1 3 ± 1 41 527.5/479 LMC X-1 XMM-1 1.3 ± 0.2 0.90 +0.01 −0.02 4.4 +0.7 −0.6 5 ± 2 41 623.9/554 Swift-1 0.8 +0.1 −0.2 0.94 +0.02 −0.03 4.7 +0.8 −1.1 5 +5 −2 44 (503.4/389) Swift-2 0.36 +0.03 −0.02

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Testing slim-disk models on the thermal spectra of LMC X-3

Cited by 62 publications

References 31 publications

Radiation spectrum of a magnetized supercritical accretion disc with thermal conduction

Radiation spectrum of a magnetized supercritical accretion disc with thermal conduction

The effect of advection at luminosities close to Eddington: The ULX in M 31

Crossing the Eddington Limit: Examining Disk Spectra at High Accretion Rates

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