Mathematics – Probability
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.1007b&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #10.07; Bulletin of the American Astronomical Society, Vol. 24, p.745
Mathematics
Probability
Scientific paper
We present results of our calculation of gamma-ray emission from starburst galaxies. Starburst galaxies are luminous in infra-red and have strong non-thermal radio emission. Since the stars in the nuclei are luminous, massive (3 -- 100M_&sun;) and have very short lifespans (10(7) -- 10(8) yrs), starburst cores have a high supernova yield. Gamma-ray emission may result from the decay of radio-isotopes created during a supernova explosion and relativistic particles accelerated by shock waves due to multiple supernova explosions or/and chaotic winds from hot stars. The probability of detecting supernova gamma-ray lines from nearby starburst galaxies has been found to be reasonably high. We discuss X-ray emission due to thermal bremsstrahlung in the supernova hot gas and low energy gamma-ray emission emitted by the relativistic electrons through Compton up-scattering off the FIR and stellar UV photons. High energy gamma-ray emission with {E} begin {array}{c}> ~ end {array} 100 MeV due to cosmic ray interactions with dense molecular clouds in the core is also considered. The ratio of the cosmic ray electron to nucleon number density derived from the gamma-ray observations of the starbursts can be used to distinguish between different theories of cosmic ray origin. Our estimates of both continuum and line emission can be compared with observations, including the OSSE observations of the starburst galaxy NGC 253. () USRA Research Associate ({) } NAS/NRC Senior Research Associate
Bhattacharya Dipen
Gehrels Neil
Ozernoy Leonid
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