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Stanford, January 27 2005
Outline
• Working concept for flare physics
• Missing knowledge in the deep atmosphere
• Nature of impulse
• Magnetar behavior
Stanford, January 27 2005
Overlapping needs…
• HE astrophysicists tell helioseismologists where the flare impulse happens
• Helioseismologists tell HE astrophysicists what sunspot magnetic fields above and below 5000 = 1 must be like
Stanford, January 27 2005
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Schrijver et al., Solar Phys. 206, 69, 2002
Stanford, January 27 2005
Four things the TRACE movie showed
• Early inward motions, prior to the eruption
• Dimming - the CME starting off
• Excitation of coupled normal modes in the arcade
• Arcade blowout
• But mainly, that the energy release is COMPACT and BRIEF
Stanford, January 27 2005
Forbes, T., JGR 105, 23,153, 2000Gallagher, P. personal communication 2004
Stanford, January 27 2005
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Archive cartoon fromGurman, 1987 - showsHE region nicely
0 -rays, magnetarrays, below = 1
Stanford, January 27 2005
Particle model uncertainties
• What is the source?
• Propagation at depth: B ~ P (not divergence-free!)
• Ad-hoc assumption about wave distribution (for pitch-angle scattering)
Stanford, January 27 2005
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MDI magnetic artifacts (D. Brown) showlocations of particle precipitation in
October 28, 2003 flare?
Stanford, January 27 2005
Energy and momentum
• Cross-sections and difficulty of inference
• Total energies in particles
• Recall Lin & Hudson 1976 (or Kane & Donnelly 1971): energetic electrons may contain the total flare energy after B2/8
Stanford, January 27 2005
Ramaty et al., ApJ 455, 193, 1995: protons can rivalelectrons for total energy
Stanford, January 27 2005
Flare/Magnetar comparison
• Flare impulse via particles above photosphere, ~1032 ergs, localized, extended in time
• Magnetar impulse via -rays below photosphere, ~1022 ergs, distributed across hemisphere, 0.2 s duration