Accretion Disks

Plasma Physics · Part 7

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Table of Contents

  1. 1.5.1 Accretion Luminosity
  2. 2.5.2 Thin Disk Theory
  3. 3.5.3 Shakura-Sunyaev α-Disk
  4. 4.5.4 Magneto-Rotational Instability (MRI)
  5. 5.5.5 Astrophysical Applications
  6. 6.Efficiency Comparison
  7. 7.5.1.1 Eddington Luminosity
  8. 8.5.2.1 Angular Momentum Problem
  9. 9.5.2.2 Viscous Angular Momentum Transport
  10. 10.5.2.3 Steady-State Accretion Rate

Key Equations

$$\boxed{L_{acc} = \frac{GM\dot{M}}{R} = \eta \dot{M} c^2}$$
$$\frac{\partial}{\partial t}(\Sigma r^2 \Omega) + \frac{1}{r}\frac{\partial}{\partial r}(\Sigma r^3 v_r \Omega) = \frac{1}{r}\frac{\partial}{\partial r}(r^2 \nu \Sigma r \frac{d\Omega}{dr})$$
$$T_{eff}(r) = \left(\frac{3GM\dot{M}}{8\pi \sigma_{SB} r^3}\right)^{1/4} \propto r^{-3/4}$$
$$-i\omega \delta v_\phi + \frac{\kappa^2}{2\Omega}\delta v_r = -\frac{k_z^2 v_A^2}{-i\omega}\delta v_\phi$$

Equations are rendered with MathJax in the PDF with professional LaTeX typesetting.

Course Context

This PDF is part of the Plasma Physics course on CoursesHub.World. Comprehensive study of the fourth state of matter. Covers single-particle motion, kinetic theory, MHD, waves and instabilities, collisional processes, magnetic and inertial confinement fusion, space a...

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