The galactic supernova rate from COMPTEL 44Ti γ-line observations

Details The galactic supernova rate from COMPTEL 44Ti γ-line observations The galactic supernova rate from COMPTEL 44Ti γ-line observations

Apr 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aipc..510...64t&link_type=abstract

THE FIFTH COMPTON SYMPOSIUM. AIP Conference Proceedings, Volume 510, pp. 64-68 (2000).

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Stellar Content And Populations, Morphology And Overall Structure, Supernovae, Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages

Scientific paper

44Ti is one of the few radioactive nuclei produced abundantly in supernovae (SNe). Because its life time is comparable to the typical time between supernovae in the Galaxy, γ-ray lines from 44Ti provide a powerful tool for the search for optically obscured supernovae that occurred during the last few 100 years. We present our analysis of COMPTEL data (Cycle 1-6), comparing γ-ray line images and flux distributions with Monte Carlo simulations of SNe in the Galaxy. Assuming standard SNe distribution models and theoretical estimates of the 44Ti yields, we constrain the Galactic supernova rate. We compare these constraints with those obtained from the historical record covering the last millennium. Relating the current supernova rate to the observed 44Ti solar abundance through chemical evolution models, agreement can be obtained only if there is a special type of supernova (e.g., helium detonations) that produces large amounts of 44Ti, but with a very low event rate. .

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