arXiv subjects

Viacheslav V. Zhuravlev

Publications and source records attributed to Viacheslav V. Zhuravlev.

6 recordsLinked to original sources

arXiv2026

A low viscosity relatively thick twisted disk in a supermassive binary black hole as a potential model of OJ 287

In this Paper we consider twisted accretion disks in supermassive binary black hole by analytical and numerical means. It is assumed that the disk orbiting around the more massive rotating component and that the disk rings are inclined with respect to the orbital plane. We use orbital parameters of the binary often employed in the precessing massive (PM) model of the well-known blazar OJ 287. Unlike our previous investigation of a similar problem, here we consider disks with both small and relatively large relative thicknesses $δ=h/r$, where $h$ is the disk's height at a typical radius $r$, as well as a range of values of the viscosity parameter, $α$, including the cases when $α\lesssim δ$. Similar to our previous results, we find that the twisted disk relaxes to a quasi-stationary state in the frame precessing with the Lense-Thirring frequency of the orbit. However, its shape is qualitatively different from that corresponding to the case of $δ=10^{-3}$ and $α=0.1$ considered in our previous work. In a disk with $δ=10^{-3}$ but $α\le 2\cdot 10^{-2}$, we find the new effect of generation of a twisting spiral wave near the resonance between a forcing frequency associated with the presence of the secondary and the Lense-Thirring frequency of a particular disk ring defined in the precessing frame. We propose an analytic theory of it, which is in a good agreement with our numerical results. This effect leads to multiple crossings of the orbit with the disk per one orbital period, which contradicts the PM model. When $δ\gtrsim 0.1$, a typical disk's inclination within the orbit of the binary is smaller than that of the orbit which results in only two crossings of the orbit with the disk per one orbital period. We suggest that the additional heating of the disk gas by the secondary-disk collisions may result in $δ\sim 0.1$.

astro-ph.HE↗

arXiv2024

Planetary migration in wind-fed non-stationary accretion disks in binary systems

An accretion disk can be formed around a secondary star in a binary system when the primary companion leaves the Main sequence and starts to lose mass at an enhanced rate. We study the accretion disk evolution and planetary migration in wide binaries. We use a numerical model of a non-stationary alpha-disk with a variable mass inflow. We take into account that the low-mass disk has an extended region that is optically thin along the rotation axis. We consider irradiation by both the host star and the donor. The migration path of a planet in such a disk is determined by the migration rate varying during the disk evolution. Giant planets may open/close the gap several times over the disk lifetime. We identify the new type of migration specific to parts of the growing disk with a considerable radial gradient of an aspect ratio. Its rate is enclosed between the type 2 and the fast type 1 migration rates being determined by the ratio of time and radial derivatives of the disk aspect ratio. Rapid growth of the wind rate just before the envelope loss by the donor leads to the formation of a zone of decretion, which may lead to substantial outward migration. In binaries with an initial separation $a\lesssim 100$\,AU migration becomes most efficient for planets with 60--80 Earth masses. This results in approaching a short distance from the host star where tidal forces become non-negligible. Less massive Neptune-like planets at the initial orbits $r_\mathrm{p} \lesssim 2$\,AU can reach these internal parts in binaries with $a \lesssim 30$\,AU. In binaries, mass loss by the primary component at late evolutionary stages can significantly modify the structure of a planetary system around the secondary component resulting in mergers of relatively massive planets with a host star.

astro-ph.EP↗

arXiv2015

Transient dynamics of perturbations in astrophysical disks

This paper reviews some aspects of one of the major unsolved problems in understanding astrophysical (in particular, accretion) disks: whether the disk interiors may be effectively viscous in spite of the absence of marnetorotational instability? In this case a rotational homogeneous inviscid flow with a Keplerian angular velocity profile is spectrally stable, making the transient growth of perturbations a candidate mechanism for energy transfer from the regular motion to perturbations. Transient perturbations differ qualitatively from perturbation modes and can grow substantially in shear flows due to the nonnormality of their dynamical evolution operator. Since the eigenvectors of this operator, alias perturbation modes, are mutually nonorthogonal, they can mutually interfere, resulting in the transient growth of their linear combinations. Physically, a growing transient perturbation is a leading spiral whose branches are shrunk as a result of the differential rotation of the flow. This paper discusses in detail the transient growth of vortex shear harmonics in the spatially local limit as well as methods for identifying the optimal (fastest growth) perturbations. Special attention is given to obtaining such solutions variationally, by integrating the direct and adjoint equations forward and backward in time, respectively. The material is presented in a newcomer-friendly style.

astro-ph.HE↗

arXiv2015

Analytical models of relativistic accretion disks

We present not a literature review but a description, as detailed and consistent as possible, of two analytic models of disk accretion onto a rotating black hole: a standard relativistic disk and a twisted relativistic disk. Although one of these models is much older than the other, both are of topical current interest for black hole studies. The way the exposition is presented, the reader with only a limited knowledge of general relativity and relativistic hydrodynamics can --- with little or no use of additional sources -- gain good insight into many technical details lacking in the original papers.

astro-ph.HE↗

arXiv2014

No Evidence for Bardeen-Petterson Alignment in GRMHD Simulations and Semi-Analytic Models of Moderately Thin, Prograde, Tilted Accretion Disks

In this paper we introduce the first results that use data extracted directly from numerical simulations as inputs to the analytic twisted disk model of Zhuravlev & Ivanov. In both numerical and analytic approaches, fully relativistic models of tilted and twisted disks having a moderate effective viscosity around a slowly rotating Kerr black hole are considered. Qualitatively, the analytic model demonstrates the same dynamics as the simulations, although with some quantitative offset. Namely, the GRMHD simulations generally give smaller variations of tilt and twist across the disk. When the black hole and the disk rotate in the same sense, the simulated tilted disk and analytic model show no sign of Bardeen-Petterson alignment, even in the innermost parts of the disk, where the characteristic time for relaxation to a quasi-stationary configuration is of the same order as the computation time. In the opposite case, when the direction of the disk's rotation is opposite to that of black hole, a partial alignment is observed, in agreement with previous theoretical estimates. Thus, both fully numerical and analytic schemes demonstrate that the Bardeen-Petterson effect may not be possible for the case of prograde rotation provided that disk's effective viscosity is sufficiently small. This may have implications in modeling of different astrophysical phenomena, such as disk spectra and jet orientation.

astro-ph.HE↗

arXiv2014

Conservative GRMHD Simulations of Moderately Thin, Tilted Accretion Disks

This paper presents our latest numerical simulations of accretion disks that are misaligned with respect to the rotation axis of a Kerr black hole. In this work we use a new, fully conservative version of the Cosmos++ general relativistic magnetohydrodynamics (GRMHD) code, coupled with an ad hoc cooling function designed to control the thickness of the disk. Together these allow us to simulate the thinnest tilted accretion disks ever using a GRMHD code. In this way, we are able to probe the regime where the dimensionless stress and scale height of the disk become comparable. We present results for both prograde and retrograde cases. The simulated prograde tilted disk shows no sign of Bardeen-Petterson alignment even in the innermost parts of the disk. The simulated retrograde tilted disk, however, does show modest alignment. The implication of these results is that the parameter space associated with Bardeen-Petterson alignment for prograde disks may be rather small, only including very thin disks. Unlike our previous work, we find no evidence for standing shocks in our simulated tilted disks. We ascribe this to the combination of small black hole spin, small tilt angle, and small disk scale height in these simulations. We also add to the growing body of literature pointing out that the turbulence driven by the magnetorotational instability in global simulations of accretion disks is not isotropic. Finally, we provide a comparison between our moderately thin, untilted reference simulation and other numerical simulations of thin disks in the literature.

astro-ph.HE↗