2013/07/31 by Aleksander Sądowski, A. Sadowski, R. Narayan +6 · 199 citations
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Angular momentum #Astrophysical Phenomena and Observations #Astrophysical jet #Astrophysics #Astrophysics and Cosmic Phenomena #Black hole (networking) #Classical mechanics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Jet (fluid) #Mechanics #Outflow #Physics #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stt1881
published in Monthly Notices of the Royal Astronomical Society 436(4), 3856-3874 (Oxford University Press) · MNRAS, in press
openalex publication_date 2013/11/16 · arxiv created 2013/11/22 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 subrelativistic 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.