Cosmic Plasma Physics

1. Front Matter

   Pages i-xix

   PDF

2. Introduction

   • Boris V. Somov

   Pages 1-4

3. Particles and Fields: Exact Self-Consistent Description

   • Boris V. Somov

   Pages 5-20

4. A Statistical Description of Cosmic Plasma

   • Boris V. Somov

   Pages 21-50

5. Propagation of Accelerated Particles in Cosmic Plasma

   • Boris V. Somov

   Pages 51-74

6. The Motion of a Particle in Given Fields

   • Boris V. Somov

   Pages 75-116

7. Wave-Particle Interactions in Cosmic Plasma

   • Boris V. Somov

   Pages 117-136

8. Coulomb Collisions of Particles in Cosmic Plasma

   • Boris V. Somov

   Pages 137-166

9. A Hydrodynamic Description of Cosmic Plasma

   • Boris V. Somov

   Pages 167-196

10. Magnetohydrodynamics of Cosmic Plasma

    • Boris V. Somov

    Pages 197-224

11. Cosmic Plasma Flows in a Strong Magnetic Field

    • Boris V. Somov

    Pages 225-246

12. MHD Waves in Cosmic Plasma

    • Boris V. Somov

    Pages 247-260

13. Discontinuous Flows in a MHD Medium

    • Boris V. Somov

    Pages 261-290

14. Evolutionarity of MHD Discontinuities

    • Boris V. Somov

    Pages 291-314

15. Particle Acceleration by Shock Waves

    • Boris V. Somov

    Pages 315-337

16. Cosmic Plasma Equilibrium in Magnetic Field

    • Boris V. Somov

    Pages 339-362

17. Stationary Flows in a Magnetic Field

    • Boris V. Somov

    Pages 363-388

18. Magnetic Reconnection in Current Sheets

    • Boris V. Somov

    Pages 389-431

19. Stationary Models of Reconnecting Current Sheets

    • Boris V. Somov

    Pages 433-461

20. Particle Acceleration in Current Sheets

    • Boris V. Somov

    Pages 463-486

of the approximation at hand will be outlined from the viewpoint of physics rather than of many possible astronomical applications. After that, as an aid to detailed understanding, please return with pencil and paper to work out the missing steps (if any) in the formal mathematics. On the basis of such an approach the student interested in modern astro­ physics, its current practice, will find the answers to two key questions: (1) what approximation is the best one (the simplest but sufficient) for descrip­ tion of a phenomenon in cosmic plasma; (2) how tO,build an adequate model for the phenomenon, for example, a solar flare. Practice is really important for understanding the theory of cosmic plasma. Related exercises (problems and answers supplemented to each chapter) to improve skill do not thwart the theory but serve to better understanding of cosmic plasma physics. As for the applications, preference evidently is given to physical processes in the solar plasma. Why? - Much attention to solar plasma physics is con­ the possibility of th~ all-round observational test of theoretical ditioned by models. This statement primarily relates to the processes in the solar atmo­ sphere. For instance, flares on the Sun, in contrast to those on other stars as well as a lot of other analogous phenomena in the Universe, can be seen in their development, i. e.

• MHD
• Plasma
• astronomy
• magnetic field
• magnetohydrodynamics
• plasma physics

• Astronomical Institute and Faculty of Physics, Moscow State University, USA

  Boris V. Somov

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