Computer Science
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...9e..31h&link_type=abstract
Supernovae: One Millennium After SN1006, 26th meeting of the IAU, Joint Discussion 9, 17-18 August 2006, Prague, Czech Republic,
Computer Science
Scientific paper
The explosion mechanisms of Type Ia Supernovae are still a matter of debate. These events occur when a white dwarf, belonging to a binary system, accretes enough mass from its companion star and reaches the Chandrasekhar mass limit. Many theoretical approaches have been proposed although, unfortunately, there are no observations sensitive enough to confirm or refute the various scenarios selected up to now. Hence, gamma-ray emission from these events would allow unique information on the explosion mechanisms since the high energy photons emitted are produced by the decay of radioactive elements, which in turn are generated when the shock wave and incinerating front, produced from the explosion, pass through the entire star. The properties of these radioactive elements provide robust information on the internal structure of the star and the possible reasons of the explosion, which also depend on the progenitor system. We present simulations, in the gamma-ray range, achieved by a 1D and 3D Monte Carlo code using a set of theoretical models which depict different scenarios. We analyze the positron and photon transport and behaviour within the expanding ejecta and provide the sufficient theoretical information for later comparison with observations. The observations will be obtained using gamma ray satellites such as ESA's Integral, of which we have been granted with observation time in the midst of having such event take place at fairly close distances.
Bravo Eduardo
Hirschmann A.
Isern Jordi
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