SLIDE SHOW 3 B changes due to transport + diffusion III -- * * magnetic Reynold number INDUCTION EQUATION B moves with plasma / diffuses through it
(a) If R m << 1 The induction equation reduces to B is governed by a diffusion equation --> field variations on a scale L 0 diffuse away on time * * with speed
(b) If R m >> 1 The induction equation reduces to and Ohm's law --> Magnetic field is “**”frozen to the plasma
1. Diffusion Start with field B 0 (x) and watch diffuse. Current density
2. Diffusion heats the corona X-ray bright points, coronal holes, coronal loops
Coronal loops -- many tiny diffusion locations
3. Diffusion allows magnetic connections to change -- eg when flux emerges
4. Diffusion converts magnetic energy to heat in a Solar Flare Sudden brightening in chromosphere & corona near sunspots
A Solar Flare TRACE -- T = 1.6 MK and 30 MK) 1. B diffuses & heats plasma to 30 MK ! 2.Heat spreads along arcade of loops, which then cool through 1.6 MK 3. The loops rise
1. If magnetic field static, then plasma can flow only along B
Example of Plasma Motions along Loops
Covered with turbulent convection cells: (1 Mm) (15 Mm) 2. Photosphere Granulation Supergranulation This carries magnetic field to edges of cells
Map of Photospheric Magnetic Field White -- towards you; Black -- away from you B is concentrated around edges of supergranule cells by flow
In close- up: B is even concentra ted at edges of granules
3. When a magnetic field erupts, the plasma is carried with it e.g. Erupting Prominence
E.g. Coronal Mass Ejection
The SUN TODAY The photo sphere (SOHO- MDI)
Magnetic field (SOHO- MDI)
Movie of magnetic field
Chromo sphere (Ha - Big Bear)
Chromo sphere (SOHO- EIT)
Corona at 1.3 MK (EIT)
Corona at 1.6 MK (EIT)
Corona at 2.3 MK (EIT)