Black hole binaries and microquasars

Zhang, Shuang‐Nan

doi:10.1007/s11467-013-0306-z

Cited by 63 publications

(58 citation statements)

References 175 publications

(241 reference statements)

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“…However, the hysteretic state transition in XRBs, i.e., the transition of the low/hard state to thermal state occurs at a luminosity much higher than that for the transition from the thermal state to low/hard state (e.g., Miyamoto et al 1995;Zhang et al 1997;Nowak et al 2002;Maccarone & Coppi 2003;Zdziarski et al 2004;Yu et al 2004;Yu & Yan 2009), is still not well understood in the frame of the above mentioned scenarios (see, e.g., Zhang 2013, for a review). In most of the previous models, the accretion mode transition is solely triggered by the dimensionless mass accretion rate (see, e.g., Narayan et al 1998;Yuan & Narayan 2014, for reviews).…”

Section: Introductionmentioning

confidence: 99%

“…However, the advection of the field in a geometrically thin (H R 1  ) is inefficient due to its small radial velocity. The magnetic diffusion timescale is about the same as the viscous timescale in a steady disk, which leads to a very weak radial field component at the surface of a thin disk (Lubow et al 1994), though some specific mechanisms were suggested to alleviate the difficulty of field advection in thin disks (Spruit & Uzdensky 2005;Lovelace et al 2009;Guilet & Ogilvie 2012, 2013Cao & Spruit 2013). The vertical field can be dragged efficiently by an ADAF (Cao 2011), because the radial velocity of ADAFs is much larger than that of a thin accretion disk (Narayan & Yi 1994.…”

Section: Introductionmentioning

confidence: 99%

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An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

Cao

2016

ApJ

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We suggest a model of the advection-dominated accretion flow (ADAF) with magnetically driven outflows to explain the hysteretic state transition observed in X-ray binaries (XRBs). The transition from a thin disk to an ADAF occurs when the mass accretion rate is below a critical value. The critical mass accretion rate for the ADAF can be estimated by equating the equilibration timescale to the accretion timescale of the ADAF, which is sensitive to its radial velocity. The radial velocity of thin disks is very small, which leads to the advection of the external field in thin disks becoming very inefficient. ADAFs are present in the low/hard states of XRBs, and their radial velocity is large compared with the thin disk. The external field can be dragged inward efficiently by the ADAF, so a strong large-scale magnetic field threading the ADAF can be formed, which may accelerate a fraction of gas in the ADAF into the outflows. Such outflows may carry away a large amount of angular momentum from the ADAF, which significantly increases the radial velocity of the ADAF. This leads to a high critical mass accretion rate, below which an ADAF with magnetic outflows can survive. Our calculations show that the critical luminosity of the ADAF with magnetic outflows can be one order of magnitude higher than that for a conventional ADAF, if the ratio of gas to magnetic pressure 4 b~in the disk. This can naturally explain the hysteretic state transition observed in XRBs.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

Cao

2016

ApJ

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“…It includes active galactic nuclei (AGNs, H. Krawczynski and E. Treister) [1] that host super-massive black holes, stellar-size black hole X-ray binaries (BHXBs, S.-N. Zhang) [2], gamma-ray bursts (GRBs, N. Gehrels and S. Razzaque) [3], and various species in the neutron star (NS) zoo (A. K. Harding) [4]. The 5th planned article on supernovae and their remnants did not materialize.…”

Section: Pacs Numbersmentioning

confidence: 99%

Preface: High energy astrophysics

Zhang

Mésáros

2013

Front. Phys.

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High energy astrophysics is one of the most active branches in the contemporary astrophysics. It studies astrophysical objects that emit X-ray and γ-ray photons, such as accreting super-massive and stellar-size black holes, and various species of neutron stars. With the operations of many space-borne and ground-based observational facilities, high energy astrophysics has enjoyed rapid development in the past decades. It is foreseen that the field will continue to advance rapidly in the coming decade, with possible ground-breaking discoveries of astrophysical sources in the high-energy neutrino and gravitational wave channels. This Special Issue of Frontiers of Physics is dedicated to a systematic survey of the field of high energy astrophysics as it stands in 2013. 95.85.Nv, 95.85.Pw, 95.85.Ry, 95.85.Sz, 97.60.Lf, 97.60.Jd, 97.80.Jp, 98.62.Js High energy astrophysics is the branch of astrophysics that studies astrophysical objects that emit high energy photons (X-rays and γ-rays), and more generally, emit non-thermal photons outside the traditional optical wavelengths. By studying non-thermal emission in the universe, one can unveil the part of universe that is not in a steady state, usually originating in violent environments near compact objects, such as neutron stars and black holes of different scales. These objects, besides emitting the broad-band non-thermal electromagnetic radiation, are also believed to be emitters of other signals outside the electromagnetic channel. These multi-messenger signals include cosmic rays, neutrinos, and gravitational waves. The field of high energy astrophysics, along with cosmology and planetary sciences, is one of the three most active branches in the contemporary astrophysics. PACS numbersDuring the past decades, the field of high energy astrophysics has enjoyed a rapid development, thanks to an impressive list of space-borne and ground-based observational facilities. The currently operating space missions dedicated to high energy astrophysics include the Chandra X-ray Observatory, the X-ray Multi-Mirror Mission (XMM)-Newton, Suzaku, and the Nuclear

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“…In particular, magnetic reconnection between the magnetospheric lines of the central source and those anchored into the accretion disk resulting in the ejection of plasmons has been detected in numerical MHD studies by (see, e.g., Romanova et al 2002Romanova et al , 2011Zanni & Ferreira 2009, 2013Čemeljić et al 2013). The recent numerical relativistic MHD simulations of magnetically arrested accretion disks by Tchekhovskoy et al 2011;McKinney et al 2012;Dexter et al 2014 also evidence the development of magnetic reconnection in the magnetosphere of the BH and are consistent with our scenario above.…”

Section: Introductionmentioning

confidence: 98%

“…Fast reconnection has recently gained increasing interest also in other astrophysical contexts beyond the solar system because of its potential efficiency to explain magnetic field diffusion, dynamo process, and particle acceleration in different classes of sources and environments -from compact objects, like BHs (e.g., GL05, GL10, Giannios 2010), pulsars (e.g., Cerutti et al 2013Cerutti et al , 2014Sironi & Spitkovsky 2014), and gamma ray bursts (e.g., Zhang & Yan 2011), to more diffuse regions like the interstellar medium (ISM), intergalactic medium (IGM), and star forming regions (e.g., Santos-Lima et al 2010, 2013Leão et al 2013; see also Uzdensky 2011;de Gouveia Dal Pino & Kowal 2015;de Gouveia Dal Pino et al 2014 and references therein for reviews).…”

Section: Introductionmentioning

confidence: 99%

A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

Khiali

Pino

Valle

2015

Monthly Notices of the Royal Astronomical Society

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Recent studies have indicated that cosmic ray acceleration by a first-order Fermi process in magnetic reconnection current sheets can be efficient enough in the surrounds of compact sources. In this work, we discuss this acceleration mechanism operating in the core region of galactic black hole binaries (or microquasars) and show the conditions under which this can be more efficient than shock acceleration. In addition, we compare the corresponding acceleration rate with the relevant radiative loss rates obtaining the possible energy cut-off of the accelerated particles and also compute the expected spectral energy distribution (SED) for two sources of this class, namely Cygnus X-1 and Cygnus X-3, considering both leptonic and hadronic processes. The derived SEDs are comparable to the observed ones in the low and high energy ranges. Our results suggest that hadronic non-thermal emission due to photo-meson production may produce the very high energy gamma-rays in these microquasars.

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Black hole binaries and microquasars

Cited by 63 publications

References 175 publications

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

An Accretion Disk-Outflow Model for Hysteretic State Transition in X-Ray Binaries

Preface: High energy astrophysics

A magnetic reconnection model for explaining the multiwavelength emission of the microquasars Cyg X-1 and Cyg X-3

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