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@article{65321,
author = {Pugliese, Daniela and Stuchlík, Zdeněk},
article_number = {4},
doi = {http://dx.doi.org/10.1093/mnras/stac782},
keywords = {accretion; accretion discs; black hole physics; hydrodynamics; MHD; galaxies: active; galaxies: jets},
language = {eng},
issn = {0035-8711},
journal = {Monthly Notices of the Royal Astronomical Society},
title = {Lense-Thirring effect on accretion flow from counter-rotating tori},
url = {https://academic.oup.com/mnras/article-abstract/512/4/5895/6552135?redirectedFrom=fulltext},
volume = {512},
year = {2022}
}
TY - JOUR
ID - 65321
AU - Pugliese, Daniela - Stuchlík, Zdeněk
PY - 2022
TI - Lense-Thirring effect on accretion flow from counter-rotating tori
JF - Monthly Notices of the Royal Astronomical Society
VL - 512
IS - 4
SP - 5895-5926
EP - 5895-5926
SN - 00358711
KW - accretion
KW - accretion discs
KW - black hole physics
KW - hydrodynamics
KW - MHD
KW - galaxies: active
KW - galaxies: jets
UR - https://academic.oup.com/mnras/article-abstract/512/4/5895/6552135?redirectedFrom=fulltext
N2 - We study the accretion flow from a counter-rotating torus orbiting a central Kerr black hole (BH). We characterize the flow properties at the turning point of the accreting matter flow from the orbiting torus, defined by the condition u(phi) = 0 on the flow toroidal velocity. The counter-rotating accretion flow and jet-like flow turning point location along BH rotational axis is given. Some properties of the counter-rotating flow thickness and counter-rotating tori energetics are studied. The maximum amount of matter swallowed by the BH from the counter-rotating tori is determined by the background properties. The fast spinning BH energetics depends mostly on BH spin rather than on the properties of the counter-rotating fluids or the tori masses. The turning point is located in a narrow orbital corona (spherical shell), for photons and matter flow constituents, surrounding the BH stationary limit (outer ergosurface), depending on the BH spin-mass ratio and the fluid initial momentum only. The turning corona for jet-like flow has larger thickness, it is separated from the torus flow turning corona and it is closer to the BH stationary limit. Turning points of matter accreting from torus and from jets are independent explicitly of the details of the accretion and tori model. The turning corona could be observable due to an increase of flow luminosity and temperature. The corona is larger on the BH equatorial plane, where it is the farthest from the central attractor, and narrower on the BH poles.
ER -
PUGLIESE, Daniela and Zdeněk STUCHLÍK. Lense-Thirring effect on accretion flow from counter-rotating tori. \textit{Monthly Notices of the Royal Astronomical Society}. 2022, vol.~512, No~4, p.~5895-5926. ISSN~0035-8711. Available from: https://dx.doi.org/10.1093/mnras/stac782.
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