Detailed beta-transition rates for URCA nuclear pairs in 8-10 solar-mass stars

作者：Toki Hiroshi^*; Suzuki Toshio; Nomoto Ken' ichi; Jones Samuel; Hirschi Raphael

来源：Physical Review C, 2013, 88(1): 015806.

DOI：10.1103/PhysRevC.88.015806

We calculate beta-transition rates for URCA nuclear pairs using the sd-shell-model framework of Wildenthal [B. H. Widenthal, Prog. Part. Nucl. Phys. 11, 5 (1984)] with the modified Hamiltonian. We consider many beta transitions including excited states necessary for electron capture and beta decay with high Fermi energy of electrons at high electron density rho Y-e and temperature T relevant for the massive star and super-asymptotic-giant-branch star evolution. We provide beta-transition rates for URCA nuclear pairs (A = 23, 25, and 27) in the range of density 8.0 %26lt; log(10)rho Y-e %26lt; 9.2 in steps of 0.02 (Y-e is the electron mole number and rho is the nucleon density in units of g cm(-3)) and temperature 8.0 %26lt; log(10)T %26lt; 9.2 in steps of 0.05 (T is the temperature in units of K). This fine mesh is able to provide clearly the URCA density at log(10)rho Y-e = 8.92 for A = 23 and at log(10)rho Y-e = 8.81 for A = 25, while the URCA density is not clear for A = 27. For the evolution of 8-10M(circle dot) stars, the use of the fine mesh is found to increase the cooling effect and affects the final fate of these stars.

• 出版日期2013-7-15