3rd RHESSI/NESSI WORKSHOP
Distribution Functions of Energetic Flare Particles
Glasgow, Scotland, March 30- April 1, 2005

http://www.astro.gla.ac.uk/users/eduard/rhessi/workshop3/

Organisers
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LOC: John Brown (Chair), Lyndsay Fletcher,
Joe Khan, Eduard Kontar (Secy), Alec MacKinnon
+ for SOC: Gordon Emslie, Hugh Hudson, Michele Piana

Location/facilities
-------------------
The meeting will be held in the Dept. of Physics and Astronomy,
Kelvin Building, University of Glasgow [founded 1451 - past
Professors include Alexander Wilson (Wilson Effect), James Watt,
Lord Kelvin, and Peter Sweet.

Ample internet access will be available via our terminals and for
participants' laptops though the main aim is personal scientific
interaction.

The city of Glasgow offers excellent eating, drinking, art, music,
sport and science facilities (including the UK's best Planetarium
which opened Feb 2002) + outings to the nearby highlands, castles etc

(NOTE - We will give general advice in response to travel and
accomodation queries but cannot get involved in bookings etc.)

Glasgow Travel and Accommodation
--------------------------------
The city airport is served by several transatlantic carriers (at
least American, Continental and British) and several direct European
connections while nearby Prestwick supports various transatlantic
charter companies. There are fast and frequent direct air, rail, and
coach services to London, Manchester and other UK destinations.

Meeting Arrangements
--------------------
The meeting will focus on key topics/problems related to the ultimate
aim of RHESSI - i.e. how far can we go in quantitative determination
(inference) of the (spectral, space, time) distribution functions of
energetic flare electrons and ions from Hard X-Ray, gamma-ray, and
other data, starting from raw observations. Pure theory, model
fitting, flare phases and such data morphology, are discouraged
except where they bear on the diagnostic approach.

Team 1: FROM RAW DATA TO PHOTON DISTRIBUTIONS
- Instrumental calibration and background effects.
- Line and continuum issues
- Images, spectra and spectral images, bearing in mind temporal
   variation/modulation
- Direct use of modulation data as opposed to reconstructions

Team 2: FROM PHOTONS TO RADIATION SOURCE STRUCTURE
- Photon spectra and images -> radiation source (volume or line of
  sight integrated) particle distributions.
- Inversion and forward fitting approaches.
- Effects of method and cross section and albedo.

Team 3: FROM SITES OF RADIATION TO PARTICLE SOURCES
- Particle energy loss, pitch angle scattering and dispersion, drifts
- Mapping through realistic coronal magnetic models
- Particle "escape" onto open magnetic lines
- Energy and particle transport

PARTICIPATION
Attendance will be restricted to around 25-35 to allow ample time for
focussed discussion, rather than spending the meeting entirely on
presentations. All interested individuals should therefore register
their interest, before January 15, 2005 by email to eduard (at) astro.gla.ac.uk

by completing, cutting, and pasting the form below. A
final selection of attendees, and decisions on Team Leaders will be
made by the end of January on the basis of the relevance of the
contributions offered and overall meeting balance.

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NAME _______________________

INSTITUTE _______________________

Email _______________________

Phone/Fax _______________________

My active contribution to the specific topic are of this meeting would be:
as follows (Brief Topic Title + summary in not more than 200 words)

which I see as fitting best in Team ..... Second choice team ....

If accepted, the likelihood of my being able to attend is: %

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