xxth GENERAL ASSEMBLY OF IUGG VIENNA (AUSTRIA)

IAGA NEWS N0.29
DIVISION IV - SOLAR WIND AND INTERPLANETARY FIELD
GAM4.1 General Contributions
Tamas I Gombosi, Space Physics Research Laboratory,
Department for Atmospheric, Oceanic and Space
Sciences, The University of Michigan, 2455 Hayward
Avenue, Ann Arbor .Michigan 48109, USA [Fax: 313 863
5567]
GAM4. 2 Reporter Reviews
Tamas I Gombosi, Space Physics Research Laboratory,
Department for Atmospheric, Oceanic and Space
Sciences, The University of Michigan, 2455 Hayward
Avenue, Ann Arbor Michigan 48109, USA [Fax: 313 863
5567]
There will be invited reviews summarizing the latest results
in the following areas: solar wind interaction with come ts;
solar wind interaction with Mars and Venus; shocks in the
heliosphere; turbulence in the heliosphere, in the Sun and in
the source regions of the solar wind; large scale structure of
the heliosphere; and solar wind interaction with the
interstellar medium.
GAM4. 3 MHD Mode1ling and Kinetic Simulations as Tools of
Heliospheric Physics
Raymond J Walker, Space Science Center, Institute of
Geophysics & Planetary Physics, 6843 Stichter Hall,
405 Hilgard Avenue, Los Angeles CA 90024-1567, USA .
[Fax: 213 206 8042]
A S Lipatov
H Schmidt
H Washimi
The symposium will concentrate on the use of computer
simulations as an aid in understanding heliospheric physics,
and will include presentations on simulation processes,
critical reviews of simulation results and papers on new
simulation studies. Both MHO and kinetic simulations of the
solar wind and its interaction with planets and come t s will be
presented .
GAM4.4 The Outer Heliosphere
Alan J Lazarus , Center for Space Research,
Massachusetts Institute of Technology, Cambridge MA
02139, USA. [Fax: 617 253 0861]
E Smith
L I Dorman
D S I ntrilligator
Subjects include (but not limited to) the global morphology of
the heliosphere; the termination shock, the h e liopause, and
the outer shock; observational evidence (from the solar wind,
cosmic rays, radio and UV) related to the structure and/or
dynamics of the heliosphere; a nd observations use d to infer
the properties of the local interstellar medium.
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