Solar Wind

Plasma Physics · Part 7

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Table of Contents

  1. 1.1.1 Parker's Solar Wind Model
  2. 2.1.2 The Parker Spiral
  3. 3.1.3 Weber-Davis MHD Wind
  4. 4.1.4 The Heliosphere
  5. 5.1.5 Energy Budget of the Solar Wind
  6. 6.1.1.1 Why the Corona Must Expand
  7. 7.1.1.2 Derivation of Parker's Equation
  8. 8.1.1.3 Critical Point Analysis
  9. 9.1.1.4 Solution Topology
  10. 10.1.1.5 Solar Wind Parameters at 1 AU

Key Equations

$$\frac{dp}{dr} = -\frac{\rho G M_\odot}{r^2}$$
$$v = c_s \quad \text{and} \quad \frac{2c_s^2}{r_c} = \frac{GM_\odot}{r_c^2}$$
$$\tan\psi = \frac{2.7\times10^{-6} \times 1.5\times10^{11}}{4\times10^5} \approx 1 \quad \Rightarrow \quad \psi \approx 45°$$
$$\dot{J} = \dot{M}\,\Omega\, r_A^2$$

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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