The excitation of spectra in the envelopes of supernovae at late times by the deposition of positrons and γ-rays

Details The excitation of spectra in the envelopes of supernovae at late times by the deposition of positrons and γ-rays The excitation of spectra in the envelopes of supernovae at late times by the deposition of positrons and γ-rays

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980aipc...63...49m&link_type=abstract

AIP Conference Proceedings, Volume 63, pp. 49-74 (1980).

Physics

Atomic Physics

3

Supernovae, Elementary Particle Processes

Scientific paper

The excitation of spectra in the envelopes of supernovae at late times by the deposition of positrons and γ-rays is reviewed. It is shown that the species concentrations are determined by the high energy positrons or Compton electrons. Most of the energy of the secondary electrons created in the ionization process by the high energy primary electrons is deposited in the electron gas. The temperature of the electron gas is determined by the rate of energy deposition by the secondary electrons and the rate of cooling by radiation. In Type I Supernovae envelopes at late times, the principal source of cooling is forbidden line radiation. In Type II Supernovae envelopes, charge and energy transfer collisions with H+ and He+ may be important in determining the excitation and ionization states of the minor species. The outstanding problems in atomic physics and spectroscopy that limit the application of this model to the excitation of spectra in supernovae envelopes are indicated.

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