Final plenary session, April 8 Emslie * Web sites via group, and presentations individually Group 1, electron acceleration and propagation: Holman * Spectral inversion: Software exists, contact Anna Massone; f(E) coming soon. DEM(T) not useful. Piana-Massone working on regularized inversions of images, and Eamon Scullion is working towards inversion from counts spectra directly * Albedo: Jana Kasparova applications. survey of CL variation => effect at 20 keV, but not at higher energies. Dips in f(E) explainable by albedo. Use the correction. Or pileup? Lin: don't believe it is pileup, thinks the correction is correct. Theoretical interest. July 23 the only example; hump in f(E) at 65 keV? * Polarization: 15+-4% is the Emslie interpretation of McConnell's SNR; Suarez via Ge-Ge scattering also consistent with zero, but angle definitions agree with McConnell's * Footpoint size: Visibilities and forward fit (15-Jan-2005) larger footpoints have larger fluxes - several flares consistent with F ~ L^2 * Return currents: SHS, break energy variations (Zharkova movie) Emslie: looks different from the pivot-point behavior * Height dependence: great Eiffel-tower cartoon (Aschwanden); footpoint density variation enhanced chromosphere * Source motions: early impulsive flares (Sui) at low energies; parallel downward motions in a double source; upward motions consistent with evaporation. Ad hoc density model OK but not self-consistent * Anisotropic distribution functions: Kontar inversions; Aschwanden timing update. TOF not yet doable with RHESSI. Neupert delay * DC electric fields: Onel complicated VG circuit models... * Termination shock: Aurass interpretation of Oct. 28 2003, but in wrong position - controversial * Shock drift acceleration of electrons: Mann 2.8^8, 40 MK injection, V_A only 610 km/s, 10^20 cm^-2 * Constraints, discussed privately and publically with theory group. Bad cartoon shown yet again. Quack! Hudson: what about downward motions? Group 2, ion acceleration and interactions (Share) * Good interactive sessions, 3 S/C + neutrons * Jan 20 2005, Coronas 60 MeV delay. Beware of particle effects > 5,6 min after onset. Extended 511 keV flux shows D/N drop but associate this with local production due to particles but > 20 MeV a real occultation? * Sa"m's nice movie of Jan. 20, showing footpoints in the late phase * s ~ 2.6-2.8, alpha/p ~ 0.1-0.5? Pion component from Coronas (Kurt) * Debrunner, Vilmer, history of "tail" emission (long durations) * GLE rapid onset @ South Pole. Possibility of RHESSI direct neutron detection? * GR imaging: Hurford maps show 2.2 at one footpoint; displacement is the rule. Now 3 flares from October 03 series, plus Jan. 20 * October 28 event: INTEGRAL and multi-wavelength. Line narrowing. Confusogram discussion (Schrijver draft paper) attempting to relate many kinds of observation * Neutron spectrum: Tsumeb * Doppler shifts: loop tilt consistent with polarization measurement? * Time dependence of gamma-ray lines: 11C and 18F on short time scales; for 511 keV; Fe 800 keV line best for long time scales * Relationship to HXR: Shih correlations of 300 keV and 2.2. Is it better than the correlations with lower-energy HXR or even SXR? * Delays: Dauphin-Vilmer theory * Proton spectral information: nice plots of contribution functions for Ne, other, 2.2 lines vs spectral index models... Historically, the June 4 1991 event suggest a rollover at 150 MeV or so, not inconsistent with typical SEP observations * Submm: MacKinnon calculation shows not enough from positrons Henoux: impact polarization due either to few-hundred keV protons or to return-current electrons, 3 flares Miroshnichenko: Density enhancements in photosphere => 2.2 time profile Group 3, radio (White and few helpers) * Cool, dense flare (Bastian et al. 24-oct-01 event), "impulse response" event perhaps involving Razin suppression. OVRO data. "Reverse delay" in a monolithic loop as it evolves in (T, n_e). Model may not self- consistently treat evaporation. * RHESSI-Nobeyama 17-Jun-03 late hard component. Beautiful correlations! * Connectivity: "single-loop paradigm" for RHESSI suggests that 3 sources in one event would be two footpoints and one loop top. Radio helps to clarify this. * Matching light curves in well-separated sources * 10-Mar-04 excellent RHESSI/NRO match in images * 3-Nov-03 01:00 event movie, loop top at 25 keV but complete loop, with footpoints, at radio * 4-Nov-03 "X45" SST mm-wave excess (Kaufmann et al. 2004). Could positrons from pion decay produce this component? Optically thick ff? Source size estimate? * Type 3 RS pattern (Aschwanden cartoon) * 17-Mar-02 (Yan, Pick et al.) type III swarm and lateral feature in CME, idea of 10-fold compression associated with type IIIs * Pascal St-Hilaire simulations suggest upgoing electrons should be visible, but obscured by the footpoint. 29-event survey using the limb => no examples yet. Conclude that the type III electrons are not energetically significant * Farnik search for HXR from RS events, eg 27-May-02 05:03:04. Sample of 22 such events but does not believe that there is a correlation Group 4, multiwavelength (Fletcher) * Fe feature, survey of 30 RHESSI flares for EQW * ... scribe dozes a bit, material too familiar, sorry but see the detailed copious WG4 notes... * DEM from MCMC Pint-of-Ale hocus-pocus and discussion * Vaananen XSM calibrations * Mason prominence motions correlated with parallel FP motion, all via EIT observations (cf Grigis-Benz) * Milligan RHESSI/CDS evaporation (M2.2, C9.1) * Temmer 17-Jan-05 analysis RHESSI/H-alpha favors higher local reconnection rates (vertical umbral fields??), some peculiar motions * Veronig 18-Nov-03 again finds HXR favoring local reconnection rates Zharkova - see my JGR paper 2005 * Fivian energy deposition vs position * Ji "flare shear" observations * Bone occulted flare of 20-Jul-02 * Battaglia "coronal SHS", cf RHESSI science nugget suggests intrinsic * Grigis model of SHS * Warmuth/Mann SDA, lively discussion regarding interpretation of flare fast-mode shock observability - Pick prefers Moreton-wave interpretation to reconnection-outflow * Van Driel/Goff * Dennis energetics from October 2003 series: a surprisingly nice correlation * Hudson WLF Group 5, theory (Loukas) * Constraints - Efficiency of acceleration unusual except maybe in GRBs - Number problem - Problem with models - Directivity and albed - Shape of electron distribution - SHS evolution pattern - return-current model - ion/electron displacement - Electron-dominated events - SEP relationship * Scribe is slowing down, sorry - Loukas listed 14 constraints, whereas my list above only captured 10 * Zharkova RCS orbits * Young people: Grigis, Onofri, Dauphin - Grigis: two free parameters are not enough for an SHS description - Onofri: current sheet as an accelerator modeled as incompressible MHD and test particles - Dauphin: trap-plus-precipitation, possibly good cartoon * Demoulin - Where will R happen in a 3D geometry? Sweet... Skeleton field concept - Classification of skeletons, global bifurcations - QSL, hyperbolic flux tube The Book May/June draft outline made by Emslie, Dennis, Lin July/August modifications to same September/October next workshop announced November 2006ff chapter authors solicit contributions Spring 2007 next workshop, focus on the Book Summer 2007 writing Late 2007 submit to SSR Fall 2006 RHESSI/Nessie Imaging Spectroscopy Spring 2007 RHESSI VII Late 2007 RHESSI/Nessie WS I. Spectroscopy