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
Plasma activation activation: non-transferred and transferred electric arcs. In the non-transferred technique, both electrodes are part of the plasma source. One of them also acts as a gas nozzle producing a stream of plasma. After the plasma stream leaves the arc region, the ions recombine quickly, leaving the hot gas having high concentrations of chemically active hydrogen, nitrogen and oxygen atoms and compounds, which is also called remote plasma. The temperature of this gas stream is of the order of 200 – 500 C. The gas is very reactive allowing high surface treatment speeds when only a short-time contact with the substrate