Physics 681: Solar Physics and Instrumentation – Lecture 21 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research.

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Physics 681: Solar Physics and Instrumentation – Lecture 21 Carsten Denker NJIT Physics Department Center for Solar–Terrestrial Research

November 15, 2005Center for Solar-Terrestrial Research Magnetism  Fields and Conducting Matter The Induction Equation Electrical Conductivity on the Sun Frozen Magnetic Field The Magnetic Force  Flux Tubes Concentration of Magnetic Flux Tubes Observational Evidence for Flux Tubes Vertical Thin Flux Tubes Curved Thin Flux Tubes Thermal Structure of Photospheric Tubes  Sunspots  The Solar Cycle

November 15, 2005Center for Solar-Terrestrial Research Fields and Conducting Matter  Magnetic features: sunspots, sunspot fine structure, filaments, prominences, …  Magnetism on the Sun occurs on all scales! (small flux tubes to mean field)  Maxwell’s equations (magnetic permeability μ = 4π  Vs/Am)  Ohm’s law

November 15, 2005Center for Solar-Terrestrial Research  Induction equation  Magnetic diffusivity  Magnetic Reynolds number  High conductivity:  Electrical conductivity of a fully ionized gas

November 15, 2005Center for Solar-Terrestrial Research  ln Λ ≈ 5 for the solar interior, ln Λ ≈ 10 for the chromosphere, and ln Λ ≈ 20 for the corona  Conductivity is large:  The temperature in the solar photosphere/chromosphere is low  hydrogen and helium are neutral BUT heavier elements with low ionization potentials still donate electrons  collisions of electrons with neutrals  conductivity is greatly reduced  Conductivity for weak ionization  Large horizontal gradients (e.g., sunspots)  Collisions are rare and magnetic fields are strong  anisotropy  Plasma turbulence reduces conductivity

November 15, 2005Center for Solar-Terrestrial Research Kopecký and Soytürk (1971)

November 15, 2005Center for Solar-Terrestrial Research Frozen Magnetic Fields  High conductivity σ = 1 V/A (in sunspots), typical velocity v = 1 km/s, and scale height l = 100 km  frozen field lines  Total magnetic flux  Differential flux at two instances separated by an infinitesimal time interval dt

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