By Miller D. D.
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Extra info for A. H. Clifford: The first sixty-five years
Shimojo & Shibata (2000) and Shimojo et al. (2001) concluded that most X-ray jets are evaporation flows resulting from flare heating due to reconnection. In this scenario the acceleration mechanism is the gas pressure force and the jets are ejected with velocities comparable to the sound speed. UV polar jets' initial speeds are considerably higher than the sound speed (Cs,uy ~ 215 km s -1) suggesting that they are accelerated by the magnetic force. Two magnetic force acceleration scenarios have been considered in literature and both are supported by observations of UV jets.
1999). 7• gives a slow velocity of 400 km s -1. 5x1012 at 1 AU. Here S ~ / S o = 2152Snr. These were derived without considering the so-called critical point. Velocity and Energy Flux Distribution Figure 1 shows the fast wind velocity calculated from mass conservation p VS = (p VS)e that matches the reliable observed average polar density in the minimum phases (Saito 1970). As the non-radial expansion function, we assume far(r) =-- r - 2 S ( r ) / S ( 1 ) -- 1 + (Sn~ - 1)sin[ 89 1)/(r0 - 1)] for r _< ro and fur(r) = Snr for r > ro (r - z / R o ) .
9Rc < r < Rc at any height z. g. a > 0) and outer (a < 0) parts of the cross section at each height. g. at r ~ 0 the inner-a predominates. Note that values of Ez are not critical. It is easily shown that the damping of the energy flux occurs whether Ez > 0 or Ez < O. I thank Drs. T. Watanabe and S. R. Cranmer for discussions, particularly on the solar wind. B. , 518, 937 (1999). , J. , 104, 19766 (1999). H. , 100, 21677 (1995). , in Plasma Astrophysics, C. Chiuderi and G. ), p. 31, Springer (1996).