Energy losses and scattering of fast electrons in a dense plasma

1993 ◽  
Vol 36 (9) ◽  
pp. 905-908
Author(s):  
V. I. Boiko ◽  
E. A. Gorbachev
Keyword(s):  
Dense Plasma ◽  
Energy Losses ◽  
Fast Electrons

The Energy Losses of Fast Electrons

1937 ◽  
Vol 52 (10) ◽  
pp. 1035-1039 ◽  
Author(s):  
L. Laslett ◽  
D. Hurst
Keyword(s):  
Energy Losses ◽  
Fast Electrons

Total cross sections for radiational losses and radiational energy losses by fast electrons

1969 ◽  
Vol 26 (5) ◽  
pp. 522-522
Author(s):  
E. L. Stolyarova ◽  
V. V. Samedov ◽  
S. N. Volodin
Keyword(s):  
Cross Sections ◽  
Energy Losses ◽  
Total Cross Sections ◽  
Fast Electrons

Energy Losses of Fast Electrons in Nitrogen

1965 ◽  
Vol 43 (12) ◽  
pp. 4535-4536 ◽  
Author(s):  
J. Geiger ◽  
W. Stickel
Keyword(s):  
Energy Losses ◽  
Fast Electrons

Dense plasma heating and shock wave generation by a beam of fast electrons

2015 ◽  
Vol 22 (10) ◽  
pp. 102704 ◽  
Author(s):  
E. Llor Aisa ◽  
X. Ribeyre ◽  
S. Gus'kov ◽  
Ph. Nicolaï ◽  
V. T. Tikhonchuk
Keyword(s):  
Shock Wave ◽  
Dense Plasma ◽  
Plasma Heating ◽  
Wave Generation ◽  
Fast Electrons ◽  
Shock Wave Generation

scholarly journals Some Aspects of Radio Pulsar Evolution

1992 ◽  
Vol 128 ◽  
pp. 39-41
Author(s):  
V. S. Beskin ◽  
A. V. Gurevich ◽  
Ya. N. Istomin
Keyword(s):  
Neutron Star ◽  
Dense Plasma ◽  
Radio Pulsar ◽  
Energy Losses ◽  
Complete Suppression ◽  
Plasma Energy ◽  
Longitudinal Current ◽  
Pulsar Evolution ◽  
Good Agreement

It is shown that pulsar statistics are in good agreement with the theory of current (plasma) energy losses of a neutron star. Up to now two theories of pulsar braking have been considered. The first well known model is connected with the radiation of vacuum magneto-dipole waves (Ostriker and Gunn 1969). However, according to the electrodynamical theory of pulsars, the presence of a rather dense plasma in the magnetosphere of a neutron star leads inevitably to a complete suppression of magneto-dipole losses—the dynamics of the stellar slow down is determined by the longitudinal current only (Beskin, Gurevich, and Istomin 1983).

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