Team 3: FROM SITES OF RADIATION TO PARTICLE SOURCES

Draft report (.pdf file)

Working group themes

1. Particle propagation through "realistic" magnetic fields: energy loss, pitch angle scattering and dispersion, drifts
2. Particle radiation from "realistic" magnetic fields: trapping, coronal sources
3. Footpoint physics: positrons, ribbons, evaporation

Working group membership (click on the name for that worthy's abstract). The names are divided provisionally into affinity groups, around which we should have short presentations and lengthier discussions, perhaps the former in WG3 plenary meetings and the latter dispersed.

1. Galloway, Gordovskyy, Hannah, Melnikov, Petrosian

2. Fletcher Gallagher Hudson Mann McTiernan Warmuth

3. Allred Brown Murphy Ryan Veronig Woods

(e-mail list)

Organizational concept (more words about it):

This is only one of several RHESSI workshops, which continue according to this this schedule. We have is a pretty well-focused group in a small workshop here. Thus I believe that we can keep the formal presentations to a minimum and get on with real workshop work as quickly as possible. I'd suggest five minutes each in order to leave maximal time for broader discussions on specific topics.

Organizational remarks:

The "more words" link above actually describes a couple of research papers (or maybe just technical reports) that we could actually think about writing or starting at the workshop. Please think of other ones if these don't seem suitable.

The schedule for team 3 sessions will be hammered out at the first meeting, but the current idea is the following. We have three "focus area" themes. We should go through these in sequence according to a well-determined plan, so that interested parties can drift in out out. Each topic area should have about an hour's session time, so that individuals can make relevant brief comments and we can have some discussion as a group. Then, in subsequent sessions, we can either meet as a group or break up into smaller units for actual work. The Common Room in Kelvin Hall has tables, snack machines, and Kelvin's celebrated pitch diffusion experiment.

Region selection:

Since our group will deal with magnetic modeling, and since we have at least one particpant able to do that (Jim McTiernan) we need to get him started on one or preferably two active regions that would be suitable. By suitable, I think we need something near disk center with RHESSI and TRACE flare observations, and especially with first-rate magnetic data. Please make suggestions about this if you have any good candidates.

AR 486 (October-November 2003). This produced the big flares, and Tom Metcalf notes the existence of good magnetogram data for this region. There are summary pages for these "Halloween 2003" events.

2003 Oct 29 AR 0486 20:49 UT X10.0

Other Metcalf suggestions:

2003 Jan 10 AR 0242 23:36 UT C2.5

2002 Dec 16 AR 0226 22:45 UT M1.9 RHESSI: Decay phase only; lower priority

2002 Nov 20 AR 0198 17:16 UT M1.4 RHESSI: Decay phase only; lower priority

2002 Nov 12 AR 0180 17:58 UT C9.9

Lyndsay Fletcher suggestion:

2002 Jul 15 AR 0030 19:59 UT X3.0

Vahe Petrosian suggestion:

2003 Nov 3 09:43 X3.9 (see the Liu et al. preprint - Vahe's comment is that this event has a simple morphology).

Eduard Kontar suggestion:

2002 Aug 21 01:41 M1.4 - a good interplanetary event at ~W45

---

Hugh Hudson (hhudson@ssl.berkeley.edu)