Western Michigan University1, Physics, Kalamazoo, MI 48009 Northern Michigan University2, Physics Student, Marquette, MI 49855
Heavy nuclei abundances in the universe are not attributed to normal stellar burning processes. Nearly all are thought to be a result of the astrophysical r- and s- processes. Thirty-five remaining nuclei cannot be produced through b-decay and consequently are not a result of neutron capture. These p-nuclei are likely due to ?-induced reactions on heavier, stable nuclei in shock fronts of type II supernovae. They could also be the result of deflagration flame fronts in type I supernovae or O-Ne burning zones of massive stars. Regardless of the p-process site, understanding the processes responsible for these p-nuclei are heavily dependent their nuclear properties.
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