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

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 general advice in response to travel 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 (led by Richard Schwartz,TBC)
- 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 (led by Chris Johns-Krull)
- 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 (led by Hugh Hudson)
- 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

Attendance
----------
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 5, 2004 by email to eduard@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 mid-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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