Energy, momentum and mass outflows and feedback from thick accretion discs around rotating black holes

By A. Sa̧dowski, Ramesh Narayan, R. Penna, Yucong Zhu. 2013

163 citations recorded by the source corpus.

Using long-duration general relativistic magnetohydrodynamic simulations of radiatively inefficient accretion discs, the energy, momentum and mass outflow rates from such systems are estimated. Outflows occur via two fairly distinct modes: a relativistic jet and a sub-relativistic wind. The jet power depends strongly on the black hole spin and on the magnetic flux at the horizon. Unless these are very small, the energy output in the jet dominates over that in the wind. For a rapidly spinning black hole accreting in the magnetically arrested limit, it is confirmed that jet power exceeds the total rate of accretion of rest mass energy. However, because of strong collimation, the jet probably does not have a significant feedback effect on its immediate surroundings. The power in the wind is more modest and shows a weaker dependence on black hole spin and magnetic flux. Nevertheless, because the wind subtends a large solid angle, it is expected to provide efficient feedback on a wide range of scales inside the host galaxy. Empirical formulae are obtained for the energy and momentum outflow rates in the jet and the wind.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/24e782359eafc4be8289be63cc1a217841b53c64

How researchers see this paper

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In Astronomy and Astrophysics

1. Ramesh Narayan
2. A. Tchekhovskoy
3. A. Sa̧dowski
4. F. Yuan
5. J. McKinney
6. B. Metzger
7. E. Quataert
8. D. Kasen

In Nuclear and High Energy Physics

1. Ramesh Narayan
2. A. Sa̧dowski
3. A. Tchekhovskoy
4. F. Yuan
5. J. McKinney
6. Yucong Zhu
7. Harvard
8. E. Quataert

Citations in the corpus

• Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, result): “Because of these differences, the results of previous work that focused on the sub-relativistic disk outflow (e.g., Narayan et al. 2012; Sa̧dowski et al. 2013) are not directly applicable to the merger problem .”
• Hot Accretion Flows Around Black Holes (2014, methodology): “Typically, the jet dominates the energy output, whereas the wind dominates the momentum output (Yuan et al. 2012a, Sadowski et al. 2013a).”
• First M87 Event Horizon Telescope Results. V. Physical Origin of the Asymmetric Ring (2019, unknown): “Models with 1f ~ are conventionally referred to as Standard and Normal Evolution (SANE; Narayan et al. 2012; Saḑowski et al (2013a)) models; models with maxf f~ are conventionally referred to as Magnetically Arrested Disk (MAD; Igumenshchev et al. 2003; Narayan et al. 2003) models.”
• Three-dimensional simulations of supercritical black hole accretion discs - luminosities, photon trapping and variability (2015, methodology): “The simulations described in this paper were performed with the general relativistic radiation magnetohydrodynamical (GRRMHD) code KORAL (Sądowski et al. 2013) which solves the conservation equations in a fixed, arbitrary spacetime using finite-difference methods.”
• NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, methodology): “Sadowski et al. (2013) compared the power of the wind and the jet and found that, if the black hole spin and magnetic flux at the horizon are large, jet power will usually dominate the wind power.”
• Numerical simulations of super-critical black hole accretion flows in general relativity (2013, methodology): “The M1 closure scheme employed here is approximate in the sense that KORAL does not include any frequency dependence, but instead evolves the frequency integrated radiative energy density and flux, with grey opacities.”
• Global simulations of axisymmetric radiative black hole accretion discs in general relativity with a mean-field magnetic dynamo (2014, methodology): “2.1 GRRMHD code — KORAL We use the general relativistic radiation magnetohydrodynamics (GRRMHD) code KORAL (Sa̧dowski et al. 2013a, 2014), which employs a Godunov scheme to evolve the rest mass, energy and momentum conservation equations in a fixed, arbitrary spacetime using finite-difference…”
• Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, methodology): “This is probably an upper limit (see Narayan et al. 2012; Sa̧dowski et al. 2013b).”