1 20 January 2005: Session Summary SHINE 2006 Zermatt, Utah, 31 July - 4 August Invited Talks Riley: what was the Alfven speed in the corona at the onset of this event?  This CME would have had no problem driving a shock at any altitude above ~1.5 Rs; no conflict with the inferred altitudes of SEP production from neutron monitors. Zank: Can shock acceleration account for the features of this event?  Probably, but only the first steps toward a cogent simulation have been taken; lots of work needs to be done. Share: How do the RHESSI observations fit into the picture?  Tremendous progress since last year’s first report by Bob Lin  RHESSI gamma-rays shows two components:  Soft, short-duration component, coming from footpoints;  Hard, long-duration component, onset delayed by ~4minutes, no information so far on whether compact or diffuse.  The hard component is close in onset time and spectral index to the interplanetary SEPs, but contains only <0.3 % as many protons

CME (from Gopalswamy et al., 2005) V A near active region (0, 180) Riley: Alfven speeds as a function of height in vicinity of active region 720.

3 Simulated Spectra from Zank et al. 11 hours 24 hours 31 hours 36 hours (at 1 AU)

4 Maximum and injection energies Remarks: 1) Parallel shock calculation assumes wave excitation implies maximum energies comparable 3) Injection energy at Q-perp shock much higher than at Q-par therefore expect signature difference in composition

5 RHESSI SUMMARY from Gerry Share RHESSI has observed two distinct components of particle acceleration in the 2005 January 20 th solar flare. There is a ‘normal’ impulsive component beginning at ~06:42 UT, peaking at ~06:47 UT, lasting about 10 minutes, evidenced by bremsstrahlung and nuclear-line radiation interacting at a footpoint with an ion power-law index of ~-3. A separate component began with a sharp 1-2 min peak at ~06:46 UT, with a spectrum dominated by pion-decay radiation; emission lasted for ~2 hours. No information as yet on how compact this source is. The GLE event commenced at 06:48 UT and was observed at energies >4 GeV. An ~5 min-wide peak was observed at ~06:53 UT.

6 The high-energy photon emission observed by RHESSI extends up to two hours after the sharp peak. >20 MeV

7 Summary of RHESSI Results from Gerry Share Comparison of accelerated particles interacting at the Sun and observed in space (Mewaldt, priv. comm. 2005) Total number of protons >30 MeV: Solar flare impulsive component: (2.8 ± 0.8) x Solar flare high-energy component:  0.7 x Event integrated SEPs: 210 x Power-law spectral index: Solar flare impulsive component: 3.0 ± 0.05 Solar flare high-energy component: <2.3 Event integrated SEPs: 2.15

8 Session Summary SHINE 2006 Zermatt, Utah, 31 July - 4 August Poster Previews Coyner: context: exploring correlations between open flux and SEP composition; more open flux in events with high Fe/O Jackson: SMEI observations: CME is moving to the NW; but shock (and SEPs) are seen here at Earth and at Ulysses, south of the ecliptic. Tylka: context: disappearance of large Fe-rich events late in Cycle 23; connection to change in the remnant flare seed population? Evenson: update on Spaceship Earth neutron monitor measurements: event simulation requires changing interplanetary scattering conditions (from ~ 0.9 AU to ~ 0.6 AU), perhaps due to self-generated waves; no evidence of multiple injections in the source profile; noted a similarity in shape between ~GeV proton injection profile and ~500 kHz radio emission. Ryan: Milagro observations: interplanetary proton spectrum steepens at ~1 GeV from E -2 to E -3.3 ; very narrow pitch angle distribution;

9 20 January 2005 as a SHINE Campaign Event? SHINE 2006 Zermatt, Utah, 31 July - 4 August 2006 Before deciding to go forward as a campaign event, we need to hear specific proposals about what to pursue and a commitment to work on them for next year’s meeting. Some ideas came up during the session: Numerical SEP modeling, with initial conditions better tuned to this event. Time-dependent interplanetary SEP composition: can it be accounted for by transport or does it demand multiple sources for the interplanetary particles? Modeling of the radio emissions? Modeling the SMEI observations? Please give us your feedback on the post-conference evaluation form!