"Nucleosynthesis in Supernova" by Dr. Michael Famiano (WMU)

Date: November 30, 2009
Time: 4:00 p.m. - 5:00 p.m.
Location: PAD 308

Speaker: Dr. Michael Famiano (Western Michigan University)
Topic: Nucleosynthesis in Supernova.
Location: PAD 308, 4-5pm.
Abstract: The astrophysical r-process is thought to be responsible for the production of 70% of the nuclei heavier than iron and nearly all of the actinides. It occurs in the hot, neutron-rich regions of type II supernovae, and proceeds by producing heavy nuclei via neutron captures on lighter “seed” nuclei. Since the r-process is thought to be responsible for the production of nuclei a heavy as uranium, it must proceed quickly with enough available neutrons to allow it to produce these heavy nuclei. If the density of the environment is too low or if the neutron richness of the environment is not high enough, the r-process will not proceed. One possible way in which the r-process speeds up is via the rapid decays of nuclei in their excited states. The b-decays of neutron-rich nuclei in the r-process are studied for nuclei in ground states as well as in excited states as might be found in the hot thermal environment of the r-process. It is possible that r-process calculations may be successful is excited-state nuclear decays are accounted for.