【摘要】：We investigate nucleosynthesis inside the gamma-ray burst(GRB) accretion disks formed by the Type II collapsars. In these collapsars, the core collapse of massive stars first leads to the formation of a proto-neutron star. After that, an outward moving shock triggers a successful supernova. However, the supernova ejecta lacks momentum and within a few seconds the newly formed neutron star gets transformed to a stellar mass black hole via massive fallback. The hydrodynamics of such an accretion disk formed from the fallback material of the supernova ejecta has been studied extensively in the past. We use these well-established hydrodynamic models for our accretion disk in order to understand nucleosynthesis, which is mainly advection dominated in the outer regions. Neutrino cooling becomes important in the inner disk where the temperature and density are higher. The higher the accretion rate(˙M) is, the higher the density and temperature are in the disks. We deal with accretion disks with relatively low accretion rates: 0.001 M ⊙ s 1~˙M ~0.01 M ⊙ s 1and hence these disks are predominantly advection dominated. We use He-rich and Sirich abundances as the initial condition of nucleosynthesis at the outer disk, and being equipped with the disk hydrodynamics and the nuclear network code, we study the abundance evolution as matter inflows and falls into the central object. We investigate the variation in the nucleosynthesis products in the disk with the change in the initial abundance at the outer disk and also with the change in the mass accretion rate. We report the synthesis of several unusual nuclei like31P,39K,43Sc,35Cl and various isotopes of titanium, vanadium, chromium, manganese and copper. We also confirm that isotopes of iron, cobalt, nickel, argon, calcium, sulphur and silicon get synthesized in the disk, as shown by previous authors. Much of these heavy elements thus synthesized are ejected from the disk via outflows and hence they should leave their signature in observed data.
LI Zhi-hong;SU Jun;GUO Bing;LI Zhi-chang;BAI Xi-xiang;LIU Jian-cheng;LI Yun-ju;YAN Sheng-quan;WANG Bao-xiang;WANG You-bao;LIAN Gang;ZENG Shen;LI Er-tao;FANG Xiao;LIU Wei-ping;CHEN Yong-shou;SHU Neng-chuan;FAN Qj-wen;;The Astrophysical S Factors of the ~(12)C(p,γ)~(13)N Reaction[A];Annual Report of China Institute of Atomic Energy 2009[C];2010年