A Novel Jet Model: Magnetically Collimated, Radiation-Pressure Driven Jet

Takeuchi, Shun; Ohsuga, Ken; Mineshige, Shin

doi:10.1093/pasj/62.5.l43

Cited by 40 publications

(42 citation statements)

References 39 publications

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“…In addition, the magnetic fields affect the geometrical structure of jets. Takeuchi et al (2010) performed axisymmetric two-dimensional radiation MHD simulations and found that the jet is collimated by magnetic stress, while it is accelerated by radiative force. Therefore, the structure of the jet and the outflow is affected by magnetohydrodynamical processes.…”

Section: Comparison With Observations Of Ulxsmentioning

confidence: 99%

Comptonized Photon Spectra of Supercritical Black Hole Accretion Flows With Application to Ultraluminous X-Ray Sources

Kawashima

Ohsuga

Mineshige

et al. 2012

ApJ

118

140

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Radiation spectra of supercritical black hole accretion flows are computed using a Monte Carlo method by postprocessing the results of axisymmetric radiation hydrodynamic simulations. We take into account thermal/bulk Comptonization, free-free absorption, and photon trapping. We found that a shock-heated region (∼10 8 K) appears at the funnel wall near the black hole where the supersonic inflow is reflected by the centrifugal barrier of the potential. Both thermal and bulk Comptonization significantly harden photon spectra although most of the photons upscattered above 40 keV are swallowed by the black hole due to the photon trapping. When the accretion rate onto the black hole isṀ2 , where L E is the Eddington luminosity, the spectrum has a power-law component which extends up to ∼10 keV by upscattering of photons in the shock-heated region. In higher mass accretion rates, the spectra roll over around 5 keV due to downscattering of the photons by cool electrons in the dense outflow surrounding the jet. Our results are consistent with the spectral features of ultraluminous X-ray sources, which typically show either a hard power-law component extending up to 10 keV or a rollover around 5 keV. We found that the spectrum of NGC 1313 X-2 is quite similar to the spectrum numerically obtained for high accretion rate2 ) source observed with low viewing angle (i = 10Our numerical results also demonstrate that the face-on luminosity of supercritically accreting stellar mass black holes (10 M ) can significantly exceed 10 40 erg s −1 .

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Section: Comparison With Observations Of Ulxsmentioning

confidence: 99%

Comptonized Photon Spectra of Supercritical Black Hole Accretion Flows With Application to Ultraluminous X-Ray Sources

Kawashima

Ohsuga

Mineshige

et al. 2012

ApJ

118

140

View full text Add to dashboard Cite

show abstract

“…Therefore, an accretion disk threaded by ordered magnetic field lines is therefore always sub-Keplerian (Ogilvie & Livio 1998, 2001Cao & Spruit 2002;Cao 2012). Radiationmagnetohydrodynamic simulations have been carried out on the global structure of the accretion disks and outflows around black holes (e.g., Moscibrodzka et al 2007;Mościbrodzka & Proga 2009;Takeuchi et al 2010;Ohsuga & Mineshige 2011;Vaidya et al 2011). It has been found that the magnetic force, together with the radiation force exerted by accretion disks, can efficiently drive outflows from luminous accretion disks.…”

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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“…To see what force is responsible for the acceleration and collimation of the jet, we evaluate the time-averaged strengths of the vertical components of the gravitational force, the gas-pressure force, the radiation-pressure force, and the Lorentz force [13]. The result is that the jet is accelerated by the radiation-pressure force, while the Lorentz force contributes much to the collimation.…”

Section: Radiation-mhd Jetmentioning

confidence: 99%

Disk modelling by radiation-magnetohydrodynamic simulations

Mineshige

Ohsuga

Takeuchi

2012

EPJ Web of Conferences

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Abstract. Historically, various accretion models have been discussed under radially one-zone approximations. In such one-zone models, however, dynamical aspects of the accretion flow, such as internal circulation and outflows, have been totally neglected. Further, the disk viscosity is usually described by the phenomenological α-viscosity model. We, here, elucidate the theory of accretion flows and outflows based on our global, two-dimensional radiation-magnetohydrodynamic simulations, not relying on the α model. We have succeeded in producing three distinct states of accretion flow by controling only one parameter, a density normalization. Of particular importance is the presence of outflows in all three states. Several noteworthy features of the supercritical (or super-Eddington) accretion flows are found; that is, relativistic, collimated outflows (jets), and low-velocity, uncollimated outflows with clumpy structure. Observational implications are briefly discussed.

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A Novel Jet Model: Magnetically Collimated, Radiation-Pressure Driven Jet

Cited by 40 publications

References 39 publications

Comptonized Photon Spectra of Supercritical Black Hole Accretion Flows With Application to Ultraluminous X-Ray Sources

Comptonized Photon Spectra of Supercritical Black Hole Accretion Flows With Application to Ultraluminous X-Ray Sources

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

Disk modelling by radiation-magnetohydrodynamic simulations

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