Stanford, January Solar flares, magnetars, and helioseismology H.S. Hudson SSL/UCB

Stanford, January Outline Working concept for flare physics Missing knowledge in the deep atmosphere Nature of impulse Magnetar behavior

Stanford, January 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 Schrijver et al., Solar Phys. 206, 69, 2002

Stanford, January 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 Forbes, T., JGR 105, 23,153, 2000 Gallagher, P. personal communication 2004

Stanford, January Archive cartoon from Gurman, shows HE region nicely  0  -rays, magnetar  rays, below  = 1

Stanford, January 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 MDI magnetic artifacts (D. Brown) show locations of particle precipitation in October 28, 2003 flare?

Stanford, January 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 B 2 /8 

Stanford, January Ramaty et al., ApJ 455, 193, 1995: protons can rival electrons for total energy

Stanford, January  EE BremsstrahlungNuclear excitation Bad

Stanford, January Flare/Magnetar comparison Flare impulse via particles above photosphere, ~10 32 ergs, localized, extended in time Magnetar impulse via  -rays below photosphere, ~10 22 ergs, distributed across hemisphere, 0.2 s duration

Stanford, January