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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

General relativistic radiation magnetohydrodynamic simulations of thin magnetically arrested discs

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Author(s):
Teixeira, Danilo Morales [1, 2] ; Avara, Mark J. [3, 4] ; McKinney, Jonathan C. [1, 5]
Total Authors: 3
Affiliation:
[1] Univ Maryland, Dept Phys, 3114 Phys Sci Complex, College Pk, MD 20742 - USA
[2] Aeronaut Inst Technol IEFM ITA, BR-12228900 Sao Paulo - Brazil
[3] Univ Maryland, Dept Astron, 1113 Phys Sci Complex, College Pk, MD 20742 - USA
[4] Rochester Inst Technol, Ctr Computat Relat & Gravitat, Rochester, NY 14623 - USA
[5] Joint Space Sci Inst, 1113 Phys Sci Complex, College Pk, MD 27042 - USA
Total Affiliations: 5
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 480, n. 3, p. 3547-3561, NOV 2018.
Web of Science Citations: 3
Abstract

The classical, relativistic thin-disc theory of Novikov and Thorne (NT) predicts a maximum accretion efficiency of 40 per cent for an optically thick, radiatively efficient accretion disc around a maximally spinning black hole (BID. However, when a strong magnetic field is introduced to numerical simulations of thin discs, large deviations in efficiencies are observed, in part due to mass and energy carried by jets and winds launched by the disc or BH spin. The total efficiency of accretion can be significantly enhanced beyond that predicted by NT but it has remained unclear how the radiative component is affected. In order to study the effect of a dynamically relevant large-scale magnetic field on radiatively efficient accretion, we have performed numerical 3D general relativistic - radiative - magnetohydrodynamic (GRRMHD) simulations of a disc with scale height to radius ratio of H/R similar to 0.1 around a moderately spinning BH (a = 0.5) using the code HARMRAD. Our simulations are fully global and allow us to measure the jet, wind, and radiative properties of a magnetically arrested disc (MAD) that is kept thin via self-consistent transport of energy by radiation using the M1 closure scheme. Our fiducial disc is MAD out to a radius of similar to 16R(g) and the majority of the total similar to 13 per cent efficiency of the accretion flow is carried by a magnetically driven wind. We find that the radiative efficiency is slightly suppressed compared to NT, contrary to prior MAD GRMHD simulations with an ad hoc cooling function, but it is unclear how much of the radiation and thermal energy trapped in the outflows could ultimately escape. (AU)

FAPESP's process: 13/26258-4 - Superdense matter in the universe
Grantee:Manuel Máximo Bastos Malheiro de Oliveira
Support type: Research Projects - Thematic Grants