Vlad Izmodenov (team leader), Lomonosov, Moscow State University, Moscow, Russia, E-mail: firstname.lastname@example.org
Dmitry Alexashov, Institute for Problems in Mechanics,
Russian Academy of Sciences, E-mail: email@example.com
Vladimir Baranov, Institute for Problems in Mechanics, Russian Academy of Sciences, E-mail: firstname.lastname@example.org
Andrzej Czechowski, Space Research Center of the Polish Academy of Sciences, Warsaw, Poland, E-mail: email@example.com
Hans Fahr, Insitur fuer Astrophysik und Extraterrestrisch Forschung der Universitat Bonn, E-mail: firstname.lastname@example.org
Mike Gruntman, University of Southern California, Los Angeles, E-mail: email@example.com
Stan Grzedzielski, Space Research Center of the Polish Academy of Sciences, Warsaw, Poland, E-mail: firstname.lastname@example.org
Vladimir Florinski, Institute of Geophysics and Planetary Physics, University of California, Riverside, USA, E-mail: email@example.com
Reinald Kallenbach, International Space Science Institute, Bern, Switzerland, E-mail: firstname.lastname@example.org
Rosine Lallement, Service d' Aeronomie, France, E-mail: Rosine.Lallement@aerov.jussieu.fr
Yury Malama, Institute for Problems in Mechanics, Russian Academy of Sciences, E-mail: email@example.com
Ed Roelof, The Johns Hopkins University Applied Physics Lab, Laurel, MD, USA, e-mail: Edmond.Roelof@jhuapl.edu
Michael S. Ruderman, Department of Applied Mathematics, University of Sheffeld, UK, E-mail: M.S.Ruderman@sheffield.ac.uk
Peter Wurz, University of Bern, Switzerland, e-mail: firstname.lastname@example.org
Group Homepage (restricted access)
Scientific rationale of the project:
In the project we will seek the answer to the fundamental question:
What is the nature of the region of the solar wind/ LIC interaction in
the downwind direction? Or, more specifically, what physical processes
are the most important in the downwind direction? Where is the boundary
of the solar system in the downwind direction? What is the correct definition
of the heliospheric interface boundary downwind?
How do the solar wind plasma and the interstellar plasma mix? How does the heliospheric magnetic field lines evolve in the heliotail and how does it interact with the interstellar magnetic fields?
The concept of the heliospheric interface is currently rather well developed.
It has been shown in a number of works (including many papers of the participants
of this project), that the solar wind and interstellar plasmas, interplanetary
and interstellar magnetic fields, interstellar atoms, galactic and anomalous
cosmic rays (GCRs and ACRs) and pickup ions play prominent roles in the
However, most of the numerical multi-component models of the heliospheric interface do not have an extended computational region in the downwind direction. There are two reasons for this: a) in the downwind there are a number of additional physical processes whose roles need to be evaluated; b) it is commonly known, that it is difficult to perform numerical computations in the downwind regions of the interaction of gas flows with obstacles. Here we have a similar problem. This problem is due to the boundary conditions, which are quite difficult to satisfy for a sub-sonic outflow.
At the present time, the interest to the studies of the processes in the heliotail is growing due to the recent CELIAS/SOHO determination of the enhancement of high-energy ENA fluxes in the downwind direction, and new measurements of ENA fluxes by IMAGE ENA instruments. The experimental study of the ENA fluxes may provide a unique tool to probe the heliospheric tail.
In the frame of the team we study and/or evaluate the following
physical processes on the downwind plasma flow and its diagnostics: the
charge exchange process; effects connected with interstellar and heliospheric
magnetic fields; interstellar ionization; diffusion across the heliopause
by micro scale plasma processes like wave-particle interactions as well
as by turbulences in the LISM.