Secondary electron spectra in interstellar clouds, and the bremsstrahlung gamma-ray luminosity

Details Secondary electron spectra in interstellar clouds, and the bremsstrahlung gamma-ray luminosity Secondary electron spectra in interstellar clouds, and the bremsstrahlung gamma-ray luminosity

Nov 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...262..749m&link_type=abstract

Astrophysical Journal, Part 1, vol. 262, Nov. 15, 1982, p. 749-759.

Astronomy and Astrophysics

Astrophysics

35

Astronomical Models, Bremsstrahlung, Electron Spectroscopy, Gamma Rays, Interstellar Matter, Secondary Emission, Electron Energy, Electron Scattering, Particle Interactions

Scientific paper

Low energy electron spectra in interstellar clouds are calculated. The processes considered are the following: inside the cloud, secondary production (knock-on, meson decay), ionization losses and bremsstrahlung losses; outside the cloud, particle transport by convection as well as diffusion. It has been assumed that the waves that scatter the electrons are generated by low energy cosmic rays (protons and alpha-particles), which stream into the c5oud to replenish ionization losses. Hence the convection is always directed back into the cloud. The process works up to electron energies of about 300 MeV if only interactions with protons are considered, and about 600 MeV if alpha-particles are considered as well. Significant intensity enhancements are possible. Acceleration of electrons in the intercloud medium has not been considered, except for Fermi acceleration associated with the diffusive scattering across the cloud. The bremsstrahlung gamma-ray luminosity of interstellar clouds from secondary electrons is calculated

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