Formation of Overheated Regions and Truncated Disks Around Black Holes: Three-Dimensional General Relativistic Radiation-Magnetohydrodynamics Simulations

Takahashi, Hiroyuki R.; Ohsuga, Ken; Kawashima, Tomohisa; Sekiguchi, Y.

doi:10.3847/0004-637x/826/1/23

Cited by 92 publications

(92 citation statements)

References 43 publications

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“…Recent numerical simulations confirm this process as a plausible and efficient jet power extraction mechanism (e.g. Komissarov et al 2007;Tchekhovskoy et al 2010Tchekhovskoy et al , 2011McKinney et al 2012;Takahashi et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime

Inoue

Doi

Tanaka

et al. 2017

ApJ

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We study the disk-jet connection in supermassive black holes by investigating the properties of their optical and radio emissions utilizing the SDSS-DR7 and the NVSS catalogs. Our sample contains 7017 radio-loud quasars with detection both at 1.4 GHz and SDSS optical spectrum. Using this radioloud quasar sample, we investigate the correlation among the jet power (P jet ), the bolometric disk luminosity (L disk ), and the black hole mass (M BH ) in the standard accretion disk regime. We find that the jet powers correlate with the bolometric disk luminosities as log P jet = (0.96 ± 0.012) log L disk + (0.79 ± 0.55). This suggests that the jet production efficiency of η jet 1.1 +2.6 −0.76 × 10 −2 assuming the disk radiative efficiency of 0.1 implying low black hole spin parameters and/or low magnetic flux for radio-loud quasars. But it can be also due to dependence of the efficiency on geometrical thickness of the accretion flow which is expected to be small for quasars accreting at the disk Eddington ratios 0.01 λ 0.3. This low jet production efficiency does not significantly increase even if we set the disk radiative efficiency of 0.3. We also investigate the fundamental plane in our samples among P jet , L disk , and M BH . We could not find a statistically significant fundamental plane for radio-loud quasars in the standard accretion regime.

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Section: Introductionmentioning

confidence: 99%

Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime

Inoue

Doi

Tanaka

et al. 2017

ApJ

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“…During the last few years, fully general relativistic radiation MHD codes have been developed by a number of groups (Sadowski et al 2013McKinney et al 2014;Fragile et al 2014;Takahashi & Ohsuga 2015;Takahashi et al 2016). In this paper, we use one of these state-of-theart codes, KORAL (Sadowski et al 2013, to explore the super-Eddington accreting stellar-mass BH model of ULXs.…”

Section: Introductionmentioning

confidence: 99%

Spectra of black hole accretion models of ultraluminous X-ray sources

Narayan

Sądowski

Soria

2017

Monthly Notices of the Royal Astronomical Society

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We present general relativistic radiation MHD simulations of super-Eddington accretion on a 10M black hole. We consider a range of mass accretion rates, black hole spins, and magnetic field configurations. We compute the spectra and images of the models as a function of viewing angle, and compare them with the observed properties of ultraluminous X-ray sources (ULXs). The models easily produce apparent luminosities in excess of 10 40 erg s −1 for pole-on observers. However, the angle-integrated radiative luminosities rarely exceed 2.5 × 10 39 erg s −1 even for mass accretion rates of tens of Eddington. The systems are thus radiatively inefficient, though they are energetically efficient when the energy output in winds and jets is also counted. The simulated models reproduce the main empirical types of spectra -disk-like, supersoft, soft, hard -observed in ULXs. The magnetic field configuration, whether MAD ("magnetically arrested disk") or SANE ("standard and normal evolution"), has a strong effect on the results. In SANE models, the X-ray spectral hardness is almost independent of accretion rate, but decreases steeply with increasing inclination. MAD models with non-spinning black holes produce significantly softer spectra at higher values ofṀ , even at low inclinations. MAD models with rapidly spinning black holes are quite different from all other models. They are radiatively efficient (efficiency factor ∼ 10 − 20%), super-efficient when the mechanical energy output is also included (70%), and produce hard blazar-like spectra. In all models, the emission shows strong geometrical beaming, which disagrees with the more isotropic illumination favoured by observations of ULX bubbles.

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“…In the case of a/M = 0.9375, we use the simulation data of run C, where the time span is t KS = 0.08 − 0.19 sec. The mass accretion rate is sub-Eddington (Ṁ /L Edd ∼ 10 −1 ) at the whole time (see Takahashi et al 2016, section 3.1). We postulate that the emission region is located within the radial position of the inner edge of the torus; that is, r H /M ≤ R KS /M ≤ 20, where R KS = r KS sin θ KS .…”

Section: Model and Methods Of Numerical Calculationsmentioning

confidence: 99%

“…This requirement is satisfied by the implementation of the three-dimensional general relativistic radiation-magnetohydrodynamics (3D-GRRMHD) simulation (McKinney et al 2014;Mishra et al 2016;Takahashi et al 2016;Sadowski et al 2017). We use the latest simulation data of Takahashi et al (2016), and examine whether the key features assumed in paper I are reproduced.…”

Section: Introductionmentioning

confidence: 99%

High-frequency Quasi-periodic Light Variations from Arc-shaped Gas Clouds Falling onto a Black Hole

Moriyama¹,

Mineshige²,

Takahashi³

2017

ApJ

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We investigate dynamical and radiative properties of arc-shaped gas clouds falling onto a stellar mass black hole based on the three-dimensional general relativistic radiation-magnetohydrodynamics (3D-GRRMHD) simulation data. Assuming that the gas clouds radiate due mainly to the free-free emission and/or optically thick, inverse Compton scattering, we calculate how the emissivity distributions develop with time.We find that (1) gas clouds, each of which has a ring-like or arc shape, are intermittently formed, and that (2) they slowly fall to the black hole, keeping nearly the Keplerian orbital velocity. These features support the dynamical properties of the gas clouds assumed in the spin measurement method proposed by Moriyama & Mineshige (2015), but the radius of the inner edge of the accretion disk is larger than that of the marginally stable orbit (ISCO).Next, we examine how each gas cloud is observed by a distant observer by calculating the photon trajectories in the black hole space-time. The luminosity of the accretion flow exhibits significant time variations on different timescales, reflecting the time evolution of the gas density distributions. The relatively slow variations on the time durations of 0.08 − 0.10 sec is due to the formation and fall of gas clouds, while quasi-periodic flux peaks with short time intervals (0.01 sec) are due to the quasi-periodic enhancement of light from the non-axisymmetric arc-shaped clouds through the beaming effect. This may account for the high-frequency quasi-periodic oscillations (HF QPOs) observed in black hole binaries. The observational implications and future issues are briefly discussed.

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Formation of Overheated Regions and Truncated Disks Around Black Holes: Three-Dimensional General Relativistic Radiation-Magnetohydrodynamics Simulations

Cited by 92 publications

References 43 publications

Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime

Disk–Jet Connection in Active Supermassive Black Holes in the Standard Accretion Disk Regime

Spectra of black hole accretion models of ultraluminous X-ray sources

High-frequency Quasi-periodic Light Variations from Arc-shaped Gas Clouds Falling onto a Black Hole

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