Black hole binaries

McClintock, Jeffrey E.; Remillard, Ronald A.

doi:10.1017/cbo9780511536281.005

Cited by 830 publications

(751 citation statements)

References 211 publications

(336 reference statements)

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“…In addition to the above standard filters, we only used X-ray events within the energy range of 3-13 keV which translates to PCA channels 7-32. This energy range is comparable -17 -to the bandpass in which high-frequency quasi-periodic oscillations have been reported from stellar-mass black holes 10,14,15 . Moreover, beyond 13 keV the background dominates the overall count rate by a factor greater than 10.…”

Section: Methodssupporting

confidence: 57%

“…M82 X-1's previous mass estimates of a few hundred solar masses combined with the Type-C identification 2,4,9 of its mHz X-ray quasi-periodic oscillations suggest that 3:2 ratio, twin-peak, high-frequency oscillations analogous to those seen in stellar-mass black holes, if present, should be detectable in the frequency range of a few Hz 16 . We accordingly searched Rossi X-ray Timing Explorer's (RXTE's) proportional counter array archival data to look for 3:2 oscillation pairs in the frequency range of [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16] Hz which corresponds to a black hole mass range of 50-2000 M ⊙ .…”

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confidence: 99%

“…1c) to the Type-C low-frequency X-ray oscillations of stellar-mass black holes -4 -(frequency range of 0.2-15 Hz) 10,26 . There are two uncertainties with such scaling: (1) it was unclear-until now-whether these mHz oscillations are indeed the Type-C analogs of stellarmass black holes 8,9 and (2) both the Type-C and the mHz oscillations are variable, resulting in a large dispersion in the measured mass of 25-1300M ⊙ 1,2,4,6 .…”

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confidence: 99%

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A 400-solar-mass black hole in the galaxy M82

Pasham

Strohmayer

Mushotzky

2014

Nature

192

197

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The brightest X-ray source in M82 has been thought to be an intermediatemass black hole (10 2−4 solar masses, M ⊙ ) because of its extremely high luminosity and variability characteristics 1−6 , although some models suggest that its mass may be only ∼ 20 M ⊙ 3,7 . The previous mass estimates are based on scaling relations which use low-frequency characteristic timescales which have large intrinsic uncertainties 8,9 . In stellar-mass black holes we know that the high frequency quasi-periodic oscillations that occur in a 3:2 ratio (100-450 Hz) are stable and scale inversely with black hole mass with a reasonably small dispersion 10−15 . The discovery of such stable oscillations thus potentially offers an alternative and less ambiguous mass determination for intermediate-mass black holes, but has hitherto not been realized. Here, we report stable, twin-peak (3:2 frequency ratio) X-ray quasi-periodic oscillations from M82 X-1 at the frequencies of 3.32±0.06Hz and 5.07±0.06 Hz. Assuming that we can scale the stellar-mass relationship, we estimate its black hole mass to be 428±105 M ⊙ . In addition, we can estimate the mass using the relativistic precession model, from which we get a value ofOscillations arising from general relativistic effects should scale inversely with the black hole mass if they arise from orbital motion near the innermost stable circular orbit in the We detected two power spectral peaks at 3.32±0.06 Hz (coherence, Q = centroid frequency (ν)/width(∆ν) > 27) and 5.07±0.06 Hz (Q > 40) consistent with a 3:2 frequency ratio ( Fig. 1a, b). The combined statistical significance of the detection is greater than 4.7σ (see Methods for details).The proportional counter array's field of view (1 • ×1 • ) of M82 includes a number of accreting X-ray sources in addition to M82 X-1 18 . The remarkable stability of the two quasiperiodic oscillations on timescales of a few years (Movies 1 & 2), their 3:2 frequency ratio and their high oscillation luminosities strongly suggest they are not low-frequency quasi-periodic oscillations from a contaminating stellar-mass black hole (see Methods for details). Also a pulsar origin is very unlikely for several reasons. First, a pulsar signal would be much more coherent than that of the observed quasi-periodic oscillations, which clearly have a finite width. Second, based on the observed high quasi-periodic oscillation luminosities it is extremely implausible that they originate from a pulsar (see Methods for details). Finally, it would be highly coincidental to have two pulsars in the same field of view with spins in the 3:2 ratio. Also, based on the average power spectra of the background sky and a sample of accreting super-massive black holes monitored by the proportional counter array in the same epoch as M82, we rule out an instrumental origin for these oscillations 3 & 4). This leaves M82 X-1, persistently the brightest source in the field of view, as the most likely source associated with the 3:2 ratio quasi-periodic oscillation pair.We estimated M82 X-1's black hole ...

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Section: Methodssupporting

confidence: 57%

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confidence: 99%

mentioning

confidence: 99%

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A 400-solar-mass black hole in the galaxy M82

Pasham

Strohmayer

Mushotzky

2014

Nature

192

197

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“…McClintock & Remillard (2003) found that the upper QPO frequency in microquasars scales well as ν U = 2.793(M 0 /M ) −1 kHz which is in good agreement with the 1/M scaling of the first term in equation (1.1).…”

Section: Troubles With the Spin: 1/m Scalingsupporting

confidence: 76%

QPOs in Microquasars: the Spin Problem

et al. 2006

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Abstract.In Galactic microquasars with double-peak kHz quasi-periodic oscillations (QPOs), the ratio of the two frequencies is 3:2. This supports the suggestion that double-peak kHz QPOs are due to a non-linear resonance between two modes of accretion disk oscillations. For the microquasars with known mass, we briefly compare the black hole spin estimates based on the orbital resonance model with the recently reported spin predictions obtained by fitting the spectral continua. Results of these two approaches are not in good agreement. We stress that if the spectral fit estimates are accurate and can be taken as referential (which is still questionable), the disagreement between the predicted and referential values would represent a rather generic problem for any relativistic QPO model, as no spin influence would appear in the observed 1/M scaling of the QPO frequencies. The epicyclic frequencies relevant in these models are often considered to be equal to those of a test particle motion. However modifications of the frequencies due to disc pressure or other non-geodesic effects may play an important role, and the inaccuracy introduced in the spin estimates by the test particle approximation could be crucial.

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“…Resonance between such a frequency modes which proposed by Kluzniak and Abromowicz [23] can be a physical mechanism for existing Quasi-periodic oscillations (QPOs). QPOs in the X-ray fluxes of some astrophysical objects such as a neutron star and black hole sources have been reviewed by many researches including van der Klis [42] and McClintock et al [30]. Johannsen [18] has examined the radial and vertical epicyclic frequencies in the Kerr-like metric.…”

Section: Introductionmentioning

confidence: 99%

Circular orbits and accretion process in a class of Horndeski/Galileon black holes

Salahshoor

Nozari

2018

Eur. Phys. J. C

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In this paper the geodesics motion and accretion process around a subclass of Horndeski/Galileon black holes are investigated. Firstly, we present spherically symmetric geometries in a Horndeski/Galileon black hole spacetime by considering an isothermal fluid around the black hole. Then we focus on three main issues: in the first step circular orbits of test particles and their stability in equatorial plane are examined in details. Then, by treating perturbations via restoring forces, oscillations of particles around the central object are studied. Finally, the accretion process, the critical speed of the flow and accretion rate are investigated in this setup properly.

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Black hole binaries

Abstract: keV for a Crab-like spectrum with photon index Γ = 2.1. Table 4.1. Confirmed black hole binaries: primary properties Source Alternative Year b Type c Fx,max D P orb Spec. References name a (µJy d ) (kpc) (hr) 0422+32 V518 Per 1992/1 L,T 3000 2.6 ± 0.7

Cited by 830 publications

References 211 publications

A 400-solar-mass black hole in the galaxy M82

A 400-solar-mass black hole in the galaxy M82

QPOs in Microquasars: the Spin Problem

Circular orbits and accretion process in a class of Horndeski/Galileon black holes

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