Diverse Supernova Sources for ther‐Process
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Abstract
We present a simplied analysis using equations for the charge ow, which include capture, for the l e production of r-process nuclei in the context of the recent supernova hot bubble model. The role of l e capture in speeding up the charge ow, particularly at the closed neutron shells, is studied together with the b ow at freezeout and the e ect of neutrino-induced neutron emission on the abundance pattern after freezeout. It is shown that a semiquantitative agreement with the gross solar r-process abundance pattern from the peak at mass number A D 130 through the peak at A D 195 and up to the region of the actinides can be obtained by a superposition of two distinctive kinds of r-process events. These correspond to a low frequency case L and a high frequency case H, which take into account the low abundance of 129I and the high abundance of 182Hf in the early solar nebula. The lifetime of 182Hf (q 182 B 1.3 ] 107 yr) associates the events in case H with the most common Type II supernovae. These events would be mainly responsible for the r-process nuclei near and above A D 195. They would also make a signicant amount of the nuclei between A D 130 and 195, including 182Hf, but would make very little 129I. In order to match the solar r-process abundance pattern and to satisfy the 129I and 182Hf constraints, the events in case L, which would make the r-process nuclei near A D 130 and the bulk of those between A D 130 and 195, must occur D10 times less frequently but eject D1020 times more r-process material in each event.
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