A Separable Solution for the Oscillatory Structure of Plasma in Accretion Disks

Abstract

We provide a new analysis of the system of partial differential equations describing the radial and vertical equilibria of the plasma in accretion disks. In particular, we show that the partial differential system can be separated once a definite, oscillatory (or hyperbolic) form for the radial dependence of the relevant physical quantities is assumed. The system is thus reduced to an ordinary differential system in the vertical dimensionless coordinate. The resulting equations can be integrated analytically in the limit of small magnetic pressure. We complete our analysis with a direct numerical integration of the more general case. The main result is that a ring-like density profile (i.e., radial oscillations in the mass density) can appear even in the limit of small magnetic pressure.

6 pages, 4 figures. To appear in Europhysics Letters

References in corpus (2)

• Theory of magnetically powered jets
• Thermo-Rotational Instability in Plasma Disks Around Compact Objects

Cited by in corpus (5)

• Crystalline Structure of Accretion Disks: Features of the Global Model
• Non-stationary Magnetic Microstructures in Stellar Thin Accretion Discs
• Self-collimated axial jets seeds from thin accretion disks
• Behavior of thin disk crystalline morphology in the presence of corrections to ideal magnetohydrodynamics
• General features of the linear crystalline morphology of accretion disks