The Case for Hypercritical Accretion in M33 X-7

Méndez, Ernesto; Brown, G. E.; Lee, Chang-Hwan; Park, Il H.

doi:10.1086/593977

Cited by 31 publications

(27 citation statements)

References 18 publications

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“…Thus, we conclude that the spin of LMC X-1 is natal, which is the same conclusion that has been reached for three other stellar black holes Shafee et al 2006;Liu et al 2008). We note, however, that an alternative scenario for the origin of high spins for black holes in X-ray binaries has been proposed that invokes hypercritical accretion (Moreno Méndez et al 2008). …”

Section: Comprehensive Error Analysis: Final Determination Of Spin Pasupporting

confidence: 85%

A Determination of the Spin of the Black Hole Primary in LMC X-1

Gou

McClintock

Liu

et al. 2009

ApJ

151

143

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The first extragalactic X-ray binary, LMC X-1, was discovered in 1969. In the 1980s, its compact primary was established as the fourth dynamical black hole candidate. Recently, we published accurate values for the mass of the black hole and the orbital inclination angle of the binary system. Building on these results, we have analyzed 53 X-ray spectra obtained by RXTE and, using a selected sample of 18 of these spectra, we have determined the dimensionless spin parameter of the black hole to be a * = 0.92 +0.05 −0.07 . This result takes into account all sources of observational and model-parameter uncertainties. The standard deviation around the mean value of a * for these 18 X-ray spectra, which were obtained over a span of several years, is only Δa * = 0.02. When we consider our complete sample of 53 RXTE spectra, we find a somewhat higher value of the spin parameter and a larger standard deviation. Finally, we show that our results based on RXTE data are confirmed by our analyses of selected X-ray spectra obtained by the XMM-Newton, BeppoSAX, and Ginga missions.

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Section: Comprehensive Error Analysis: Final Determination Of Spin Pasupporting

confidence: 85%

A Determination of the Spin of the Black Hole Primary in LMC X-1

Gou

McClintock

Liu

et al. 2009

ApJ

151

143

View full text Add to dashboard Cite

show abstract

“…Likewise for M33 X-7 and LMC X-1, the corresponding minimum spin-up timescales are > 17 and > 25 million years, respectively, while the respective ages of the systems are < ∼ 3 and < ∼ 5 million years . It therefore appears that the spins of these systems must be chiefly natal, although possibly such high spins could be achieved during a short-lived evolutionary phase of hypercritical accretion (Moreno Méndez et al 2008). …”

Section: The High Natal Spins Of the Persistent Black Holesmentioning

confidence: 99%

Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets

2013

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The spins of ten stellar black holes have been measured using the continuumfitting method. These black holes are located in two distinct classes of X-ray binary systems, one that is persistently X-ray bright and another that is transient. Both the persistent and transient black holes remain for long periods in a state where their spectra are dominated by a thermal accretion disk component. The spin of a black hole of known mass and distance can be measured by fitting this thermal continuum spectrum to the thin-disk model of Novikov and Thorne; the key fit parameter is the radius of the inner edge of the black hole's accretion disk. Strong observational and theoretical evidence links the inner-disk radius to the radius of the innermost stable circular orbit, which is trivially related to the dimensionless spin parameter a * of the black hole (|a * | < 1). The ten spins that have so far been measured by this continuum-fitting method range widely from a * ≈ 0 to a * > 0.95. The robustness of the method is demonstrated by the dozens or hundreds of independent and consistent measurements of spin that have been obtained for several black holes, and through careful consideration of many sources of systematic error. Among the results discussed is a dichotomy between the transient and persistent black holes; the latter have higher spins and larger masses. Also discussed is recently discovered evidence in the transient sources for a correlation between the power of ballistic jets and black hole spin.

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“…We ( [5], [6], [9], [12], [13]) model binaries in which the primary star (BH progenitor) evolves as a single star until its core begins He burning. When He burning begins in the core the stellar radius expands a further 10 to 15% relative to the red giant radius, it fills its Roche Lobe and begins to transfer mass to the secondary star, i.e.…”

Section: Discussionmentioning

confidence: 99%

GRBs∕HNe from Kerr Black Holes in Binaries

Méndez

2010

AIP Conference Proceedings

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The Collapsar model, in which a massive star ( 20M ⊙ ) fails to produce a supernova (SN) and forms a black hole (BH), provides the main framework for understanding long Gamma-Ray Bursts (GRBs) and the accompanying hypernovae (HNe). However, single massive-star models that explain the population of pulsars, predict cores that rotate too slowly to produce GRBs/HNe. We present a model of binary evolution that allows the formation of Kerr BHs where the spin of the BH can be estimated from the pre-collapse orbit, and use the Blandford-Znajek (BZ) mechanism to estimate the available energy for a GRB/HN. A population synthesis study shows that this model can account for both, the long GRB and the subluminous GRB populations.

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The Case for Hypercritical Accretion in M33 X-7

Cited by 31 publications

References 18 publications

A Determination of the Spin of the Black Hole Primary in LMC X-1

A Determination of the Spin of the Black Hole Primary in LMC X-1

Black Hole Spin via Continuum Fitting and the Role of Spin in Powering Transient Jets

GRBs∕HNe from Kerr Black Holes in Binaries

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