Matter Outflows from AGN: A Unifying Model

Vilkoviskij, E. Y.; Lovelace, R. V. E.; Павлова, Л. А.; Romanova, M. M.; Yefimov, S. N.

doi:10.1007/s10509-006-9180-2

Cited by 2 publications

(5 citation statements)

References 95 publications

(98 reference statements)

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“…In the hierarchical picture of galaxy formation, the most massive dark halos with small angular momentum can account for the early formation of the most massive black holes. The SMBH forms by a centrally focused collapse entering a phase of a dense supermassive gaseous object which is supported by star-gas interactions (Bisnovatyi-Kogan & Syunyaev 1972;Vilkoviskij 1975;Hara 1978;Langbein et al 1990). The interaction of a compact stellar cluster (CSC) with a massive central object in the form of a superstar or SMBH was considered by Vilkoviskij (1975), Hills (1975), and Hara (1978).…”

Section: Introductionmentioning

confidence: 99%

“…The SMBH forms by a centrally focused collapse entering a phase of a dense supermassive gaseous object which is supported by star-gas interactions (Bisnovatyi-Kogan & Syunyaev 1972;Vilkoviskij 1975;Hara 1978;Langbein et al 1990). The interaction of a compact stellar cluster (CSC) with a massive central object in the form of a superstar or SMBH was considered by Vilkoviskij (1975), Hills (1975), and Hara (1978). The evolution of the dense non-rotating stellar cluster was studied by Spitzer & Saslaw (1966) and Bisnovatyi-Kogan (1978) among others, and the evolution of the gas sphere was considered by Langbein et al (1990).…”

Section: Introductionmentioning

confidence: 99%

“…Stellar interactions with ADs were also considered by Vilkoviskij & Bekbosarov (1982), Vilkoviskij (1983), and Syer et al (1991). More detailed investigations of the stellar orbits crossing ADs were presented in Vokrouhlicky & Karas (1998) and inŠubr & Karas (1999).…”

Section: Introductionmentioning

confidence: 99%

“…If the inner part of the AD reaches a critical surface density the interaction of orbits with the gas (or more correctly energy and momentum transfer of stars due to ram pressure effects, henceforth denoted as dissipation) cannot be neglected anymore. Stellar interactions with accretion disks were also considered by Vilkoviskij & Bekbosarov (1982); Vilkoviskij (1983); Syer et al (1991). More detailed investigations of the stellar orbits, crossing accretion disks were presented in Vokrouhlicky & Karas (1998) and in Šubr & Karas (1999).…”

Section: Introductionmentioning

confidence: 99%

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Enhanced Accretion Rates of Stars on Supermassive Black Holes by Star-Disk Interactions in Galactic Nuclei

Just

Yurin

Makukov

et al. 2012

ApJ

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We investigate the dynamical interaction of a central star cluster surrounding a supermassive black hole (SMBH) and a central accretion disk (AD). The dissipative force acting on stars in the disk leads to an enhanced mass flow toward the SMBH and to an asymmetry in the phase space distribution due to the rotating AD. The AD is considered as a stationary Keplerian rotating disk, which is vertically extended in order to employ a fully self-consistent treatment of stellar dynamics including the dissipative force originating from star-gas ram pressure effects. The stellar system is treated with a direct high-accuracy N-body integration code. A star-by-star representation, desirable in N-body simulations, cannot be extended to real particle numbers yet. Hence, we carefully discuss the scaling behavior of our model with regard to particle number and tidal accretion radius. The main idea is to find a family of models for which the ratio of two-body relaxation time and dissipation time (for kinetic energy of stellar orbits) is constant, which then allows us to extrapolate our results to real parameters of galactic nuclei. Our model is derived from basic physical principles and as such it provides insight into the role of physical processes in galactic nuclei, but it should be regarded as a first step toward more realistic and more comprehensive simulations. Nevertheless, the following conclusions appear to be robust: the star accretion rate onto the AD and subsequently onto the SMBH is enhanced by a significant factor compared to purely stellar dynamical systems neglecting the disk. This process leads to enhanced fueling of central disks in active galactic nuclei (AGNs) and to an enhanced rate of tidal stellar disruptions. Such disruptions may produce electromagnetic counterparts in the form of observable X-ray flares. Our models improve predictions for their rates in quiescent galactic nuclei. We do not yet model direct stellar collisions in the gravitational potential well of the black hole, which could further enhance the growth rate of the black hole. Our models are relevant for quiescent galactic nuclei, because all our mass accretion rates would give rise to luminosities much smaller than the Eddington luminosity. To reach Eddington luminosities, outflows, and feedback as in the most active QSOs, other scenarios are needed, such as gas accretion after galaxy mergers. However, for AGNs close to the Eddington limit, this process may not serve as the dominant accretion process due to the long timescale.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Enhanced Accretion Rates of Stars on Supermassive Black Holes by Star-Disk Interactions in Galactic Nuclei

Just

Yurin

Makukov

et al. 2012

ApJ

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“…Our theoretical approach to the problem of matter outflow from AGN was presented in Vilkoviskij & Karpova (1996), and in complete it was described in Vilkoviskij et al (1999Vilkoviskij et al ( , 2006.…”

Section: Introductionmentioning

confidence: 99%

The modelling of the line-locking effect in broad absorption line QSOs

Vilkoviskij¹,

Yefimov²

2006

Proc. IAU

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Abstract. We present a unification model of the matter outflow from AGN. The model includes calculations of the hot gas dynamics, the dynamics of the cold clouds in the hot gas flow, and the radiation transfer in this two-phase medium. We used the model for calculation of the ultraviolet spectrum of the quasar q1303+308. The spectrum of this object is a well-know example of the line-locking effect. Our model calculations permits for the first time to obtain some thin details seen in the observed absorption spectrum, which confirms the validity of the main issues of our theory and model.

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Matter Outflows from AGN: A Unifying Model

Cited by 2 publications

References 95 publications

Enhanced Accretion Rates of Stars on Supermassive Black Holes by Star-Disk Interactions in Galactic Nuclei

Enhanced Accretion Rates of Stars on Supermassive Black Holes by Star-Disk Interactions in Galactic Nuclei

The modelling of the line-locking effect in broad absorption line QSOs

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