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Lecture 3 Magneto hydrostatics

PHYS 777 Plasma Physics and Magnetohydrodynamics. 2004  Fall Instructor: Dr. Haimin Wang. Lecture 3 Magneto hydrostatics. Force Equation (2-21). pure vertical fields. Horizontal field. Cylindrically Symmetric Fields. (3-16). Pure Axial Fields. R <a. R >a. R <a. R >a.

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Lecture 3 Magneto hydrostatics

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  1. PHYS 777 Plasma Physics and Magnetohydrodynamics 2004  Fall Instructor: Dr. Haimin Wang Lecture 3Magneto hydrostatics

  2. Force Equation (2-21)

  3. pure vertical fields Horizontal field

  4. Cylindrically Symmetric Fields (3-16) Pure Axial Fields R<a R>a R<a R>a

  5. R<a gas pressure balances with magnetic pressure and tension R>a gas pressure balances with tension

  6. In lab, this configuration is called linear Pitch Relationship beween current I and number of particles / unit length —— Bennet’s Relation Force – Free Field —— linear force free

  7. Magnetostatic Fields

  8. Current – Free Fields (potential fields) Constants are determined by boundary conditions. Many codes have been developed. e.g. Fig 3.7. Use observed surface magnetic fields as boundary condition. Force-Free Fields

  9. General remarks It can be shown that (Cowling 1976) if fields have minimum energy, must be force free. However, force-free does not mean minimum energy. Virial theorem

  10. Simple constant α force free solutions J: Bessel function Non-constant α force free fields

  11. Magnetic Diffusion

  12. Homework • Estimate the scale heights in solar photosphere, transition region and corona. • A vertical magnetic flux tube should expand from photosphere to corona. If 1% of photospheric area is occupied by the magnetic fields, at what height, 100% of the surface area is occupied by magnetic fields? • Derive Bennett’s relation, starting from fundamental magnetohydrostatics equation with cylindrical symmetry.

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