Share, WG2 The tail that wags the solar dog! Model spectrum Model spectra as function of spectral index; flat (HE) spectra produce more pseudo-continuum SEP correlation: Yes, well maybe: 28-Oct and 2-Nov-03 Heliospheric connectivity maps; protons on 2.4 R_o but well-connected, whereas electrons on 1.2 R_o (Lin, Mewaldt) H, He, O spectra from ACE/GOES/SAMPEX: broken powerlaws, break at 10 MeV/nuc Alpha/proton ratio 0.3-0.5 at Sun, but only 0.03 in SEP - ? Jan 20 2005 event, hardest GLE since 1956; spectral hardness well-predicted by solar alpha/proton ratio of .5 Albert's list of 11 events, showing good correlation between 300 keV and 2.2 fluences Oct 28 Coronas data: early bursts seen to 26 MeV, but later bit above 60 MeV; infer pion production in later phase, even developing a "pion peak" but at 40 MeV. Red shift? Calibration error? Submm increasing spectrum also conceivably attributed to pi-decay positrons? Seismic waves seen via time-distance diagrams (Oct 28, Donea & Lindsey) RHESSI for Oct 28; decreasing continuum from pion-product scattering Spectral mismatch doesn't look so bad as the one Dennis and Hudson criticized Gan calculations of H-alpha inconsistent with warm chromosphere Narrow lines can't be explained by subphotospheric 2% ionization Persistet annihilation line from 2-Nov event; line shape OK with Vernazza Varying low-FIP/high-FIP ratio; average FIP looks coronal Integral reaction rate above 1 gm/cm^2 even for flat spectra (Murphy model for 4.4 line) 20-Jan-05 late phase with day/night interruption GR image shows footpoint separation of 15 arc s for 28-Oct 20-Jan find 250-keV coronal source? 511 keV images for the first time: front and rear agree, but at only 40% the flux inferred spectroscopically White, WG3 The head of the solar dog? List of presentations and joint sessions Farnik: search for "slow" reverse-drift bursts 14-aug-02; fast-drift from 31-oct-03. RHESSI 25-keV rate not well correlated and leads radio Aurass: 300 MHz spikes and HXR, example also shows radio lag @ 20% correlation Klein: 24-apr-03. MICA sees low CME lift-off; type II moves laterally underneath the CME; type IV moves out radially above flare site Dauphin: 3-nov-03, outward motion seen by SXI points to radio source locations show II _above_ CME? Images not simultaneous? " " : remarkable late continuum, well after flare/CME, broadband synchrotron shows late-phase acceleration low in corona " " : agreement between radio and HE RHESSI spectral indices, hardening to 1.6 above 1 MeV Ji and Huang: 9-Sep-02, two sources identifiable with interacting loops? HXR only in one of the loops... B asymmetry? Pitch-angle model? Kundu: 17-jun-03 RHESSI/NORP late-phase event. Loop-top polarization Vilmer: 3-nov-01 01:20, coronal HE source moving downward? Late-phase sharp radio spike, hard spectrum high turnover freq => trapping to produce radio and no HXR Bone: 20-jul-02 coronal source >100 keV; 3 estimates of density => >10^11, not enough to stop such high energies Gan: 24-aug-02 NORH loop source, ffinding initial shrinkage @ early phase Silva: SST @200, 400 GHz soon to have IR as well. 3-nov-02 and another event show anomalous increasing spectrum (typically synchro shows normal flattening at HE) (cf 4-Nov event) Theory constraints - harder spectra @ radio wavelengths - all possible flare configurations - prompt precipitation sometimes, stable trapping other times Model-independent quantities!!! Movie of 3-nov-03 flare, 17-34 GHz + RHESSI shows simple HX, complex mm: sudden spike illuminates entire radio loop! Also mm-wave jet! Holman, WG1 Inverse results... no notes at first Determination of LE cutoffs Sui: spectral flattening for early impulsive sources suggest cutoff as high as 38 keV? But what do you mean by cutoff? 2-jun-02 event; 15-apr-02 event worry about swamping thermal Theory of same: acceleration, transport (return current and trapping) Kasparova-Kontar: 31-oct-03 inverse + forward-fit. Kontar software for albedo corrections. Always should check! In this case the cutoff goes away... Kasparova survey for flat spectra; no evidence in general for F_bar cutoffs MacKinnon: return current and hot target. Emphasize that these calculations yield the minimum non-thermal energies Zharkova: return-current continuity equation => physical explanation of spectral break, but not necessarily LE cutoff Battaglia: correlation of HXR flux and spectrum; also T and em correlated with HXR flux at 35 keV Aschwanden: TOF analysis 17-Mar-02 still not possible with RHESSI for fast component; envelope delays => density on order 10^11 Aurass-Mann: impulsive-phase TS 28-sep-01 "upper and lowr TS" (see ApJ paper) Grigis: HXR footpoints along _converging_ flare ribbons. Parallel converging motion, followed by diverging? See EFBs and Arnold's cartoon 9-nov-02 event Kontar: energy-dependent spectral index McConnell: 18% at 20-40 keV, phi=79; no error bars yet but a lot of progress has been made (mu_p ~ 10+-4) Share question: is there a dip? GHo answer: it's the cutoff. GEm answer: there is a real hump at about 70 keV, it's not the cutoff GHu comment: use each detector please Zharkova comment: there is a dip, and it comes from return current Fletcher, WG4 13 permanent members, lively discussion, presentations + special sessions Dennis: Fe and FeNi; counts spectrum of two-line fits; Fe existence means thermal unambiguously; Caspi ratio vs continuum T systematic dependences McTiernan: DEM analysis, pixons-based combination of RHESSI and GOES has large systematic uncertainties still; don't readily see cooling behavior but will include CDS and XRM when available Vaananen: XSM matches GOES, inter-calibration proceeding, 24-May-04 event for example Christe: 1500 A1-C1 events, peak temp ~10 MK and/or gamma ~6 => huge energies of 10^28-30 ergs Gallagher: CDS evaporation analysis showing VDEM of flow => gentle evaporation if _assume_ 10^18 cm^2 footpoint area Schmahl: 3-Nov-03 pre-impulsive coronal source, related to nice CME @ MLSO Krucker-Balciunaite: 18-nov-03 shows rapid variability from corona >20 keV; nice movie Pick: 17-mar-02, type III sources moving out along flank of CME into open fields (PFSS model) Veronig: 3-nov-03 09:45 coronal source, shows clear downward motions for 3-4 min, while the spectrum slowly gets harder @ 20 keV Ji: 4 more examples of 'height' decrease with time, accompanied by converging footpoints Temmer: 17-jan-05, footpoint motions not really very consistent, nor a close match to "reconnection rate" (one footpoint works, the other does not?) Fletcher: UV footpoints show reconnected flux correlations on smaller scales at multiple simultaneous points in the ribbons Hudson: tiny footpoints, containing many ergs, seen in TRACE WL Henoux: 15-Jun-01 Themis results => linear polarization in impulsive phase (proton beams? electron beams?) at outer edge of ribbons Discussion: footpoint areas (Aschwanden, Vlahos, Hudson, Emslie); electric fields in Temmer's event (V/m); polarization (Benz, Henoux, Emslie) - is the discrepancy an effect of resolution or contrariwise of seeing? Have reduced data for two polarized events Vlahos, WG5 7 regular members, 4 visitors Goals: comment about conflicting data inputs List of requirements for accelerator: 1e37 e/s, 10 msec, 10's GeV, flattening @ 500 keV; SHS Energetics, revised Emslie et al. table Overall spectrum - complexity of multiple components Electron-dominated events (30-jun-91) Time-dependent spectra, eg SHS; Kontar time-dependent inversions Nonthermal pre-impulsive ("preflare" misnomer?) coronal sources (Schmahl) Particles at 1 AU: Oakley et al. 2004 must be a part of the integrated picture. Double power laws also appear in electrons at 1 AU Delays of ions from electrons, sec to 10s of sec (antique results) Radio spectral features: spike bursts, RS, but few examples. More complaints about conflicting data inputs Magnetic configurations: radio techniques essential, need FASR; see White movie Radio-quiet flare M1.0 as shown by Benz on first day - Hudson comment about absorption? Eager discussion will follow A bit of theory: incompressible MHD, E-fields from frozen state with test particles (like Turkmani's?); from 1e30 ergs get 1e34 ergs in particles! Suspect that test-particle calculations are not so good Demand for kinetic simulations! Zharkova: 3D simulations => separated beams, different spectra, but still in test-particle non-self-consistent manner Aurass standing shock cartoon: 28-oct-03. The mechanism seems reasonable, but can it solve the number problem. Again, self-consistency in the theory is needed Arzner-Vlahos new idea: something stochastic... not followed too well Summary: no unique acceleration? Shocks, stochastic E, turbulence? Complex magnetic topologies driven by photospheric motions? Discussion: Mann asks how much energy, Emslie says A10 = 1e33 ergs; Aschwanden asks why acceleration is treated without propagation. Should there be a workshop just on that?