Bhattacharjee, Jayanta K. ; Bhattacharya, Atri ; Das, Tapas K. ; Ray, Arnab K. (2009) Quasi-viscous accretion flow - I. Equilibrium conditions and asymptotic behaviour Monthly Notices of the Royal Astronomical Society, 398 (2). pp. 841-852. ISSN 0035-8711
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Official URL: http://doi.org/10.1111/j.1365-2966.2009.14977.x
Related URL: http://dx.doi.org/10.1111/j.1365-2966.2009.14977.x
Abstract
In a novel approach to studying viscous accretion flows, viscosity has been introduced as a perturbative effect, involving a first-order correction in the α-viscosity parameter. This method reduces the problem of solving a second-order non-linear differential equation (Navier–Stokes equation) to that of an effective first-order equation. Viscosity breaks down the invariance of the equilibrium conditions for stationary inflow and outflow solutions, and distinguishes accretion from wind. Under a dynamical systems classification, the only feasible critical points of this ‘quasi-viscous’ flow are saddle points and spirals. On large spatial scales of the disc, where a linearized and radially propagating time-dependent perturbation is known to cause a secular instability, the velocity evolution equation of the quasi-viscous flow has been transformed to bear a formal closeness with Schrödinger's equation with a repulsive potential. Compatible with the transport of angular momentum to the outer regions of the disc, a viscosity-limited length-scale has been defined for the full spatial extent over which the accretion process would be viable.
Item Type: | Article |
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Source: | Copyright of this article belongs to Royal Astronomical Society. |
ID Code: | 133879 |
Deposited On: | 30 Dec 2022 11:47 |
Last Modified: | 30 Dec 2022 11:47 |
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