Physics
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.3.72v&link_type=abstract
"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,
Physics
Scientific paper
We demonstrate that the solar wind origin problem can have only one evolutionary solution. It is not known when and how the solar wind started to blow, but there are evidences that it existed on the geological time scale and will continue to exist even during crossing of dense galactic arms by the Sun in future. The Hayashi phase or the ignition of the thermonuclear burning could be an evolutionary benchmark in this respect, but details are not elaborated. It is also often assumed as plausible (but not proven) in available macroscopic and kinetic plasma theories that the solar wind exists because of the hot and dense corona with high pressure of gas and magnetic fields from one side near the Sun and rarefied low density, low temperature and low magnetic fields in the interstellar medium surrounding the Sun from the other side. Nevertheless, all these conditions are compatible both with inflow (accretion) and outflow (breeze and wind) branches of the same quasi steady politropic model solution of the Bernoulli equation without jumps considered by Bondi (1952) and Parker (1957). The solution of the quadratic equation is twice eroded and can only depict, but not predict the situation, which is totally prescribed by initial and boundary conditions at the star and in the interstellar medium around it. The definitive answers to the posed questions can be found only based on time dependent theories and observations. The magnetic, thermal and gravitational pumping of the material in the atmosphere of the star can proceed (and observed indeed) in both directions - away from the star and towards the star along finite (convective) or infinite (outflow/inflow) trajectories in kinetic or fluid approximations. Microphysical, macro-physical and global processes on the Sun and sun-like stars are non-locally and non-linearly coupled in a complicated way described by dimensionless scaling based on dissipative MHD and plasma kinetic equations with radiation. The question about possible existence of solar-like stars with accretion of the plasma will be addressed. This possibility does not contradict any physical laws. Such objects should be searched on the sky with Doppler EUV measurements.
The work was supported by the grants RFBR 07-02-00147, 06-05-64500, NSh-1255.2008.2. It is also fulfilled as a part of the Programs of the Russian Academy of Sciences: "Origin and evolution of stars and galaxies" (P-04), "Solar activity and physical processes in the Sun-Earth system" (P-16, Part 3) and "Plasma processes in the Solar system" (OFN-16).
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