Solar wind Dryer, A self-consistent solution of the three-fluid model of the Solar Wind. Astrophys. J., 222 (2), 689-695, 1978. S. Cuperman and N. Metzler, Comments on Acceleration of Solar Wind He++3 effects of Resonant and nonresonant interactions with transverse waves. J. Geophys. Res. 84 (NA5), 2139-2140 (1979) N. Metzler, S. Cuperman, M. Dryer and P. Rosenau, A time-dependent two-fluid model with thermal conduction for Solar Wind. Astrophys. J., 231 (3) 960-976, 1979. Solar wind The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona. This plasma consists of mostly electrons, protons
Relativistic plasma light. (About 10% of protons would have formula_3 at a temperature of 481 MeV - 5.6 TK.) Still higher energies are necessary to achieve a quark–gluon plasma. The primary changes in a plasma's behavior as it approaches the relativistic regime is slight modifications to the equations which describe a non-relativistic plasma and to collision and interaction cross sections. The equations may also need modifications to account for pair production of electron-positron pairs (or other particles at the highest temperatures). A plasma double layer with a large potential drop and layer separation, may accelerate electrons to relativistic velocities, and produce synchrotron