P-process nucleosynthesis inside supernova-driven supercritical accretion disks

We investigate p-process nucleosynthesis in a supercritical accretion disk around a compact object of 1.4 M[odot]. Supercritical accretion is expected to occur in a supernova (SN) with fallback material accreting onto a nascent compact object. We find that appreciable amounts of p-nuclei are synthesized via the p-process in the disk when the accretion rate M > 1.6 x 106((LEdd)/(c2)), where LEdd is the Eddington luminosity. Abundance profiles of p-nuclei ejected from SSASs have similar features to those of oxygen/neon layers in the Type II SNe when composition of the fallback gas is initially those of the oxygen/neon layers in the progenitor. The overall abundance profile is in agreement with that of the solar system. Some p-nuclei, such as Mo, Ru, Sn, and La, are underproduced in SSADs as in Type II SNe. If the fallback gas is mixed with a small fraction of proton, significant amounts of 92Mo and 138La are produced inside SSADs. 96Ru, 113Sn, and 114Sn are also abundantly produced when the fallback gas contains abundant proton though the overall abundance profile of p-nuclei is rather different from that of the solar system