2011/08/03 by Jameel-Un Nabi, Muneeb-Ur Rahman · 1 citation
Physics and Astronomy · #nucl-th #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1103/physrevc.75.035803
published as Phys. Rev. C 75, 035803 (2007) · 13 pages, 3 figures
arxiv created 2011/08/03 · arxiv updated 2011/08/04
Electron captures on nuclei play an important role in the collapse of stellar core in the stages leading to a type-II supernova. Recent observations of subluminous Type II-P supernovae (e.g. 2005cs, 2003gd, 1999br) were able to rekindle the interest in 8 - 10 which develop O+Ne+Mg cores. We used the proton-neutron quasiparticle random phase approximation (pn-QRPA) theory to calculate the B(GT) strength for 24Mg → 24Na and its associated electron capture rates for incorporation in simulation calculations. The calculated rates, in this letter, have differences with the earlier reported shell model and Fuller, Fowler, Newman (hereafter F2N) rates. We compared Gamow-Teller strength distribution functions and found fairly good agreement with experiment and shell model. However, the GT centroid and the total GT strength, which are useful in the calculation of electron capture rates in the core of massive pre-supernova stars, lead to the enhancement of our rate up to a factor of four compared to the shell model rates at high temperatures and densities.