Mechanisms and sites for astrophysical gamma ray line production

Details Mechanisms and sites for astrophysical gamma ray line production Mechanisms and sites for astrophysical gamma ray line production

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978grsa.rept....7r&link_type=abstract

In its Gamma Ray Spectry. in Astrophys. p 7-41 (SEE N78-31971 22-88)

Astronomy and Astrophysics

Astrophysics

3

Astrophysics, Emission Spectra, Gamma Ray Astronomy, Gamma Rays, Line Spectra, Electron-Positron Pairs, Energetic Particles, Galactic Radiation, Inelastic Collisions, Interstellar Matter, Positron Annihilation, Supernovae

Scientific paper

The production of gamma ray lines and estimates of line fluxes resulting from nuclear deexcitations, positron annihilation, and electron capture at various astrophysical sites are discussed. Supernova and nova explosions synthesize long-lived radioactive isotopes and eject them into space where they produce observable gamma ray lines by decaying into excited levels of daughter nuclei or by emitting positrons. Energetic charged particles in the interstellar medium, in supernova remants, in solar or stellar flares, and possibly in the vicinity of compact objects, produce gamma-ray lines by inelastic collisions which either excite nuclear levels or produce positrons and neutrons. Energetic particles can result from acceleration in time-varying magnetic fields (solar flares) or from gravitational accretion onto neutron stars and black holes. Electromagnetic processes in the strong magnetic fields of pulsars can produce positron-electron pairs, with line emission resulting from positron annihilation. Deexcitations of quantized states in strong magnetic fields can also produce lines.

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