Propagation of waves in a medium with high radiation pressure. I. Basic equations and the case of a homogeneous medium

Бисноватый-Коган, Г. С.; Блинников, С. И.

doi:10.1007/bf01007444

Cited by 88 publications

(105 citation statements)

References 4 publications

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“…The existence of a corona of hot (T ∼ 10 9 K) plasma in Cygnus X-1 was first proposed by Bisnovatyi-Kogan & Blinnikov (1977). If the corona is supported by the magnetic field and the escape of the particles occurs by diffusion instead of advection to the black hole, there is time for thermalization, and ions and electrons share the same temperature, in contrast to the advection-dominated cases (ADAFs, Narayan & Yi 1995).…”

Section: Corona Of Cygnus X-1mentioning

confidence: 99%

Coronal origin of the polarization of the high-energy emission of Cygnus X-1

Romero

Vieyro

Chaty

2014

A&A

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Context. Cygnus X-1 is the candidate with the highest probability of containing a black hole among the X-ray binary systems in the Galaxy. It is also by far the most often studied of these objects. Recently, the International Gamma-Ray Astrophysics Laboratory Imager on board the Integral satellite (INTEGRAL/IBIS) detected strong polarization in the high-energy radiation of this source, between 400 keV and 2 MeV. This radiation has been attributed to a jet launched by the black hole. Aims. We consider whether the corona around the black hole might be the site of production of the polarized emission instead of the jet. Methods. We studied self-consistently the injection of nonthermal particles in the hot, magnetized plasma around the black hole. Results. We show that both the high-energy spectrum and polarization of Cygnus X-1 in the low-hard state can originate in the corona, without needing to invoke a jet. We estimate the degree of polarization in the intermediate state, where there is no jet, to provide a tool to test our model. Conclusions. Contrary to the commonly accepted view, the jet might not be the source of the MeV polarized tail in the spectrum of Cygnus X-1.

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Section: Corona Of Cygnus X-1mentioning

confidence: 99%

Coronal origin of the polarization of the high-energy emission of Cygnus X-1

Romero

Vieyro

Chaty

2014

A&A

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“…It has also been suggested that the outflow can be accelerated by the radiation pressure of the disk (e.g., Bisnovatyi-Kogan & Blinnikov 1977;Shlosman et al 1985;Murray et al 1995). This scenario is especially attractive for the jets in the sources accreting at high mass rates.…”

Section: Introductionmentioning

confidence: 99%

The Outflows Accelerated by the Magnetic Fields and Radiation Force of Accretion Disks

Cao¹

2014

ApJ

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The inner region of a luminous accretion disk is radiation-pressure-dominated. We estimate the surface temperature of a radiation-pressure-dominated accretion disk, Θ = c 2 s /r 2 Ω 2 K (H/r) 2 , which is significantly lower than that of a gas-pressure-dominated disk, Θ ∼ (H/r) 2 . This means that the outflow can be launched magnetically from the photosphere of the radiation-pressure-dominated disk only if the effective potential barrier along the magnetic field line is extremely shallow or no potential barrier is present. For the latter case, the slow sonic point in the outflow will probably be in the disk, which leads to a slow circular dense flow above the disk. This implies that hot gas (probably in the corona) is necessary for launching an outflow from the radiation-pressure-dominated disk, which provides a natural explanation for the observational evidence that the relativistic jets are related to hot plasma in some X-ray binaries and active galactic nuclei. We investigate the outflows accelerated from the hot corona above the disk by the magnetic field and radiation force of the accretion disk. We find that with the help of the radiation force, the mass loss rate in the outflow is high, which leads to a slow outflow. This may be why the jets in radio-loud narrow-line Seyfert galaxies are in general mildly relativistic compared with those in blazars.

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“…The general view of a relatively low density hot corona and a cold accretion disk was presented by Bisnovatyi-Kogan & Blinnikov (1977). The mechanism for heating the corona may be magnetic reconnection of field loops emerging from the disk (Galeev et al 1979).…”

Section: Introductionmentioning

confidence: 99%

Non-thermal processes around accreting galactic black holes

Romero

Vieyro²,

Vila³

2010

A&A

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Context. Accreting black holes in galactic X-ray sources are surrounded by hot plasma. The innermost part of these systems is likely a corona with different temperatures for ions and electrons. In the so-called low-hard state, hot electrons Comptonize soft X-ray photons from the disk that partially penetrates the corona, producing emission up to ∼150 keV, well beyond the expectations for an optically thick disk of maximum temperature ∼10 7 K. However, sources such as Cygnus X-1 produce steady emission up to a few MeV, which is indicative of a non-thermal contribution to the spectral energy distribution. Aims. We study the radiative output produced by the injection of non-thermal (both electron and proton) particles in a magnetized corona around a black hole. Methods. Energy losses and maximum energies are estimated for all types of particles in a variety of models, characterized by different kinds of advection and relativistic proton content. Transport equations are solved for primary and secondary particles, and spectral energy distributions are determined and corrected by internal absorption. Results. We show that a local injection of non-thermal particles can account for the high energy excess observed in some sources, and we predict the existence of a high-energy bump at energies above 1 TeV, and typical luminosities of ∼10 33 erg s −1 . Conclusions. High-energy instruments such as the future Cherenkov Telescope Array (CTA) can be used to probe the relativistic particle content of the coronae around galactic black holes.

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Propagation of waves in a medium with high radiation pressure. I. Basic equations and the case of a homogeneous medium

Cited by 88 publications

References 4 publications

Coronal origin of the polarization of the high-energy emission of Cygnus X-1

Coronal origin of the polarization of the high-energy emission of Cygnus X-1

The Outflows Accelerated by the Magnetic Fields and Radiation Force of Accretion Disks

Non-thermal processes around accreting galactic black holes

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