Physics
Scientific paper
Aug 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985icrc....1..365h&link_type=abstract
In NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 1 p 365-368 (SEE N85-33902 22-93)
Physics
1
Annihilation Reactions, Diffuse Radiation, Galactic Cosmic Rays, Nuclear Fusion, Supernovae, Ejecta, Electrons, Interstellar Gas, Positrons, Relativistic Particles, Shock Waves
Scientific paper
The propagation of MeV positrons in the outer ejecta of type I supernovae was investigated. It was found that the positrons created at times of approx 100 days propagated along magnetic field lines in the outer ejecta without any appreciable pitch-angle scattering or excitation of hydromagnetic waves. The lack of significant pitch-angle scattering is well consistent with models of wave excitation and scattering by resonant interactions. This occurs because time periods to scatter the particles or to excite waves are significantly longer than escape times. Thus it is expected that, when positrons are not coupled to the ejecta by Coulomb collisions, they escape from the relatively cold, dense ejecta and reside predominantly in the tenuous, hotter, shock-heated interstellar gas. In the tenuous shock-heated gas the positron lifetime against annihilation is much greater than lifetimes in the dense ejectra. Thus the production of steady-state diffuse annihilation radiation by some fraction of these escaped positrons seems probable.
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