PUGLIESE, Daniela and Zdeněk STUCHLÍK. Relating Kerr SMBHs in active galactic nuclei to RADs configurations. Classical and Quantum Gravity. 2018, vol. 35, No 18, p. "185008-1"-"185008-54", 54 pp. ISSN 0264-9381. Available from: https://dx.doi.org/10.1088/1361-6382/aad713.
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Basic information
Original name Relating Kerr SMBHs in active galactic nuclei to RADs configurations
Authors PUGLIESE, Daniela (380 Italy, guarantor, belonging to the institution) and Zdeněk STUCHLÍK (203 Czech Republic, belonging to the institution).
Edition Classical and Quantum Gravity, 2018, 0264-9381.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United Kingdom of Great Britain and Northern Ireland
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19240/18:A0000251
Organization unit Faculty of Philosophy and Science in Opava
Doi http://dx.doi.org/10.1088/1361-6382/aad713
UT WoS 000442442000002
Keywords in English black hole physics; gravitation; hydrodynamics; accretion; accretion disks; galaxies: active; galaxies: jets
Tags International impact, Reviewed
Links GB14-37086G, research and development project. GJ16-03564Y, research and development project.
Changed by Changed by: RNDr. Jan Hladík, Ph.D., učo 25379. Changed: 4/4/2019 08:17.
Abstract
There is strong observational evidence that many active galactic nuclei (AGNs) harbour super-massive black holes (SMBHs), demonstrating multi-accretion episodes during their life-time. In such AGNs, corotating and counterrotating tori, or strongly misaligned disks, as related to the central Kerr SMBH spin, can report traces of the AGNs evolution. Here we concentrate on aggregates of accretion disks structures, ringed accretion disks (RADs) orbiting a central Kerr SMBH, assuming that each torus of the RADs is centered in the equatorial plane of the attractor, tori are coplanar and axi-symmetric. Many of the RAD aspects are governed mostly by the spin of the Kerr geometry. We classify Kerr black holes (BHs) due to their dimensionless spin, according to possible combinations of corotating and counterrotating equilibrium or unstable (accreting) tori composing the RADs. The number of accreting tori in RADs cannot exceed n = 2. We present list of 14 characteristic values of the Kerr BH dimensionless spin a governing the classification in whole the black hole range 0 <= a <= M, uniquely constrained by the RAD properties. The spin values are remarkably close providing an accurate characterization of the Kerr attractors based on the RAD properties. RAD dynamics is richer in the spacetimes of high spin values. One of the critical predictions states that a RAD tori couple formed by an outer accreting corotating and an inner accreting counterrotating torus is expected to be observed only around slowly spinning (a < 0.46 M) BHs. The analysis strongly binds the fluid and BH characteristics providing indications on the situations where to search for RADs observational evidences. Obscuring and screening tori, possibly evident as traces in x-ray spectrum emission, are strongly constrained, eventually ruling out many assumptions used in the current investigations of the screening effects. We expect relevance of our classification of Kerr spacetimes in relation to astrophysical phenomena arising in different stages of AGNs life that could be observed by the planned x-ray satellite observatory ATHENA (Advanced Telescope for High ENergy Astrophysics).
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