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HK: Physik der Hadronen und Kerne

HK 51: Kern- und Teilchen- Astrophysik IV

HK 51.8: Vortrag

Donnerstag, 25. März 1999, 16:00–16:15, C

Presupernova and Supernova Weak Rates for Nuclei (A = 18 to 100) — •Jameel-Un Nabi and H.V. Klapdor-Kleingrothaus — Max-Planck-Institut für Kernphysik, P.O. Box 103980, D-69029 Heidelberg, Germany

Weak interaction rates (e^± capture, β^± decay, (anti)neutrino energy loss rates, gamma heating rates, energy rates of β-delayed protons/neutrons, and, probability of β-delayed particle emission processes) are calculated for the first time for nuclei (A = 18 to 100) at high temperatures (0.01×10⁹ ≤ T(K) ≤ 30×10⁹) and densities (10≤ ρ Y_e(gcm⁻³) ≤ 10¹¹) using proton-neutron quasiparticle random phase approximation theory. We did the calculations for some 700 nuclei. Our calculation of stellar weak rates for fp-shell nuclei is the first extensive calculation taking nuclear structure details into account. Stellar weak rates have wide ranging applications in many astrophysical problems. Collapse of 8- 10  M⊙ stars, element synthesis, r-, s-, p-processes, and hot CNO cycles are some processes where beta transitions occur at high temperatures and densities. Some of the applications of our calc! ulated rates are also discussed.