By M. R. Kundu (auth.), Mukul R. Kundu, Gordon D. Holman (eds.)
`...will be most dear as a reference and a precis of present theoretical paintings in magnetic reconnection and plasma physics of sunlight flares and astrophysical jets. ...recommended to libraries and to plasma physicists of all persuasions.'
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Additional resources for Unstable Current Systems and Plasma Instabilities in Astrophysics: Proceedings of the 107th Symposium of the International Astronomical Union Held in College Park, Maryland, U.S.A., August 8–11, 1983
10, pp. 459-462. : 1980; J. Geophys. Res. 85, pp. 7679-7696. : 1982, J. Geophys. Res. 87, pp. 2147-2158. : 1980, J. Geophys. Res. 85, 7803-7810, 1980. : 1980, Geophys. Res. Lett. 7, pp. 917-920. : 1983, J. Geophys. Res. submitted. : 1979, Nature, pp. 243-246. : 1982, J. Geophys. Res. 87, pp. 2159-2168. E. Krieger Publ. , Malabar, Florida. : 1976, Physics of Solar Planetary Environments, pp. C. 40 c. T. : 1982, Nature 300, pp. 23-26. : 1983, J. Geophys. Res. submitted •. : 1978, Space Sci. Rev. 22, pp.
This frame 1S often referred to as the de Hoffmann-Teller (dHT) frame. The principal advantage of this procedure is that, in the moving frame, a particle either conserves its energy or changes it in a known manner in response to the electric potential structure, ¢(x), of the current sheet. In particular, reflected particles must have the same energy before and after reflection. As illustrated in Figure 5 for a symmetric field-reversing current sheet with ¢ = 0, a particle moving with guiding-center velocity v toward the sheet in the stationary frame appears to be moving alo;~g the magnetic field with guiding-center velocity v' and pitch angle a in the dHT frame (Fig.
The passage of one of these twisted tubes has been called a flux. transfer event. Similar twisted tubes, or flux ropes, are formed at Venus by velocity shear. These tubes become so highly twisted that they become kink unstable. The presence of the kink instability suggests a way of creating compound flux ropes as have been postulated to be necessary to explain photospheric magnetic structure. 1. INTRODUCTION Reconnection in astrophysical plasmas is difficult to treat theoretically and difficult to study observationally.
Unstable Current Systems and Plasma Instabilities in Astrophysics: Proceedings of the 107th Symposium of the International Astronomical Union Held in College Park, Maryland, U.S.A., August 8–11, 1983 by M. R. Kundu (auth.), Mukul R. Kundu, Gordon D. Holman (eds.)