Speaker
Mr
Masamitsu Mori
(Kyoto University)
Description
Massive stars cause huge explosions called core collapse supernovae(CCSNe) at the end of their evolution. A CCSNe is one of the strongest explosion, which releases 10 percent of the star's mass of the solar in some 10's of seconds. Most of this energy is released as neutrinos.The four fundamental interactions of nature are involved in CCSNe, and CCSNe are complex and difficult to model theoretically. Neutrinos carry information about the stellar core, so neutrino detectors around the world are waiting for a CCSNe nearby the earth. The Super-kamiokande(SK) water Cherenkove detector is also continuously monitoring for CCSNe. If a CCSN happens in our galaxy, SK can detecte about 10,000 events over more than 10 seconds. However, most theoretical simulations concentrate on only the first 1 second, which determines whether the explosion successes. Therefore, we can not compare a theory and observation when a galactic supernova is detected. For galactic supernova in near future, a long time simulation is needed. An integrated framework is being developed, which simulates supernova neutrino in one dimension from a core collapse to detection at SK.In the present study, we consider three models which lead to different neutron star models and have simulated the neutrino emission up to 20 seconds. These model have already been simulated up to 20 seconds. In this report, the difference in expected neutrino signals at SK for these models will be shown.
Primary author
Mr
Masamitsu Mori
(Kyoto University)
