Supercritical Accretion Flows around Black Holes: Two‐dimensional, Radiation Pressure–dominated Disks with Photon Trapping

Ohsuga, Ken; Mori, Masao; Nakamoto, Taishi; Mineshige, Shin

doi:10.1086/430728

Cited by 399 publications

(559 citation statements)

References 61 publications

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“…This is motivated by the possibility of gas accreting with finite angular momentum, and forming a bright nuclear disc, fed at rates well in excess of the Eddington rate (e.g. Ohsuga et al 2005;Sadowski et al 2014;Jiang, Stone & Davis 2014;McKinney et al 2014).…”

Section: Summary and Discussionmentioning

confidence: 99%

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Sakurai

Inayoshi

Haiman

2016

Mon. Not. R. Astron. Soc.

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We perform one-dimensional radiation hydrodynamical simulations to solve accretion flows onto massive black holes (BHs) with a very high rate. Assuming that photon trapping limits the luminosity emerging from the central region to L L Edd , Inayoshi, Haiman & Ostriker (2016) have shown that an accretion flow settles to a "hyper-Eddington" solution, with a steady and isothermal (T 8000 K) Bondi profile reaching 5000 times the Eddington accretion rateṀ Edd ≡ L Edd /c 2 . Here we address the possibility that gas accreting with finite angular momentum forms a bright nuclear accretion disc, with a luminosity exceeding the Eddington limit (1 L/L Edd 100). Combining our simulations with an analytic model, we find that a transition to steady hyper-Eddington accretion still occurs, as long as the luminosity remains below L/L Edd 35 (M BH /10 4 M ) 3/2 (n ∞ /10 5 cm −3 )(T ∞ /10 4 K) −3/2 (r /10 14 cm) −1/2 , where n ∞ and T ∞ are the density and temperature of the ambient gas, and r is the radius of the photosphere, at which radiation emerges. If the luminosity exceeds this value, accretion becomes episodic. Our results can be accurately recovered in a toy model of an optically thick spherical shell, driven by radiation force into a collapsing medium. When the central source is dimmer than the above critical value, the expansion of the shell is halted and reversed by ram pressure of the collapsing medium, and by shell's weight. Our results imply that rapid, unimpeded hyper-Eddington accretion is possible even if the luminosity of the central source far exceeds the Eddington limit, and can be either steady or strongly episodic.

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Section: Summary and Discussionmentioning

confidence: 99%

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Sakurai

Inayoshi

Haiman

2016

Mon. Not. R. Astron. Soc.

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“…Depending on the peak accretion rate, these episodes could occur within a day making the observation of such events rather challenging. The presence of powerful outflows, often invoked in the superEddington accretion regime (e.g., Ohsuga et al 2005, Poutanen et al 2007, Ohsuga & Mineshige 2011, Ohsuga & Mineshige 2013see also De Colle et al 2012), might make this phase even shorter by depleting matter from the disk. Such outflows coupled with the unbound stripped matter might even be able to power a nebula around the system.…”

Section: Discussion On the Mass Accretion Ratementioning

confidence: 99%

Implications of the Delayed 2013 Outburst of Eso 243-49 HLX-1

Godet

Lombardi

Antonini

et al. 2014

ApJ

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After showing four quasi-periodic outbursts spaced by ∼1 yr from 2009 to 2012, the hyper luminous X-ray source ESO 243-49 HLX-1, currently the best intermediate mass black hole (IMBH) candidate, showed an outburst in 2013 delayed by more than a month. In Lasota et al., we proposed that the X-ray light curve is the result of enhanced mass transfer episodes at periapsis from a donor star orbiting the IMBH in a highly eccentric orbit. In this scenario, the delay can be explained only if the orbital parameters can change suddenly from orbit to orbit. To investigate this, we ran Newtonian smooth particle hydrodynamical simulations starting with an incoming donor approaching an IMBH on a parabolic orbit. We survey a large parameter space by varying the star-to-black hole mass ratio (10 −5 -10 −3 ) and the periapsis separation r p from 2.2 to 2.7r t with r t , the tidal radius. To model the donor, we choose several polytropes (Γ = 5/2, n = 3/2, Γ = 3/2, n = 2, Γ = 5/3, n = 2, and Γ = 5/3, n = 3). Once the system is formed, the orbital period decreases until reaching a minimum that may be shallow. Then, the period tends to increase over several periapsis passages due to tidal effects and increasing mass transfer, leading ultimately to the ejection of the donor. We show that the development of stochastic fluctuations inside the donor by adding or removing orbital energy from the system could lead to sudden changes in the orbital period from orbit to orbit with the appropriate order of magnitude to that which has been observed for HLX-1. We also show that given the constraints on the black hole (BH) mass (M BH > 10 4 M ) and assuming that the HLX-1 system is currently near a minimum in period of ∼1 yr, the donor has to be a white dwarf or a stripped giant core. We predict that if HLX-1 is indeed emerging from a minimum in orbital period, then the period would generally increase with each passage, although substantial stochastic fluctuations can be superposed on this trend.

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“…Recent radiation (magneto-)hydrodynamic simulations predict radiation-pressure-dominated, optically thick disk winds to be driven in supercritical accretion disks (e.g., Ohsuga et al 2005;Dotan & Shaviv 2011;Ohsuga & Mineshige 2011). Although the ionized Fe-K absorption lines like those observed in Galactic BH binaries have never been observed in ultraluminous X-ray sources (ULXs; Walton et al 2012Walton et al , 2013, Middleton et al (2014) argued that uneven spectral structures often seen at »1 keV could be explained by broad blueshifted absorption lines.…”

Section: Implications For Disk Winds In Other Luminous X-ray Binariesmentioning

confidence: 99%

An Optically Thick Disk Wind in Gro J1655–40?

Shidatsu

Done

Ueda

2016

ApJ

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe revisited the unusual wind in GRO J1655−40, detected with Chandra in 2005 April, using long-term Rossi X-ray Timing Explorer X-ray data and simultaneous optical/near-infrared photometric data. This wind is the most convincing case for magnetic driving in black hole binaries, as it has an inferred launch radius that is a factor of 10 smaller than the thermal wind prediction. However, the optical and near-infrared (OIR) fluxes monotonically increase around the Chandra observation, whereas the X-ray flux monotonically decreases from 10 days beforehand. Yet the optical and near-infrared fluxes are from the outer, irradiated disk, so for them to increase implies that the X-rays likewise increased. We applied a new irradiated disk model to the multi-wavelength spectral energy distributions. Fitting the OIR fluxes, we estimated the intrinsic luminosity at the Chandra epoch was  L 0.7 Edd , which is more than one order of magnitude larger than the observed X-ray luminosity. These results could be explained if a Compton-thick, almost completely ionized gas was present in the wind and strong scattering reduced the apparent X-ray luminosity. The effects of scattering in the wind should then be taken into account for discussion of the wind-driving mechanism. Radiation pressure and Compton heating may also contribute to powering the wind at this high luminosity.

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Supercritical Accretion Flows around Black Holes: Two‐dimensional, Radiation Pressure–dominated Disks with Photon Trapping

Cited by 399 publications

References 61 publications

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity

Implications of the Delayed 2013 Outburst of Eso 243-49 HLX-1

An Optically Thick Disk Wind in Gro J1655–40?

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