Effects of β-Decays of Excited-State Nuclei on the Astrophysical r-Process
نویسنده
چکیده
A rudimentary calculation is employed to evaluate the possible effects of β-decays of excited state nuclei on the astrophysical r-process. Single particle levels calculated with the FRDM are adapted to the calculation of β-decay rates of these excited state nuclei. Quantum numbers are determined based on proximity to Excited-State β-Decays and the r-Process 2 Nilson model levels. The resulting rates are used in an r-process network calculation in which a supernova hot-bubble model is coupled to an extensive network calculation including all nuclei between the valley of stability and the neutron drip line and with masses 1≤A≤283. β-decay rates are included as functional forms of the environmental temperature. While the decay rate model used is simple and phenomenological, it is consistent across all 3700 nuclei involved in the r-process network calculation. This represents an approximate first estimate to gauge the possible effects of excited-state β-decays on r-process freezeout abundances. PACS numbers: 26.30.Hj,26.50.+x
منابع مشابه
Impact of the first - forbidden β decay on the production of A ∼ 195 r - process peak
Impact of the first-forbidden β decay on the production of A ∼ 195 r-process peak a r t i c l e i n f o a b s t r a c t First-forbidden transition Neutron emission QRPA We investigated the effects of first-forbidden transitions in β decays on the production of the r-process A ∼ 195 peak. The theoretical calculated β-decay rates with β-delayed neutron emission were examined using several astroph...
متن کاملNUCLIDES OF ASTROPHYSICS INTEREST WITH MASS NUMBERS CLOSE TO A~80 PNPI participants of the IGISOL/JYFLTRAP collaboration
Nuclei close to the N = Z line in the region near A = 80 play a special role in nuclear astrophysics since the rapid proton (rp) capture process is passing right through them (see Fig. 1). The rp-process, a sequence of rapid proton captures and β-decays, proceeds along the N = Z line up to Ni and it can continue ending in a SnSbTe cycle either in explosive X-ray bursts or in a steady state burn...
متن کاملStellar weak decay rates in neutron-deficient medium-mass nuclei
Weak decay rates under stellar density and temperature conditions holding at the rapid proton-capture process are studied in neutron-deficient medium-mass waiting-point nuclei extending from Ni up to Sn. Neighboring isotopes to these waiting-point nuclei are also included in the analysis. The nuclear structure part of the problem is described within a deformed Skyrme Hartree-Fock + BCS + quasip...
متن کاملar X iv : a st ro - p h / 98 12 24 3 v 1 1 2 D ec 1 99 8 Nuclear astrophysics
Nuclear astrophysics is that branch of astrophysics which helps understanding the Universe, or at least some of its many faces, through the knowledge of the microcosm of the atomic nucleus. It attempts to find as many nuclear physics imprints as possible in the macrocosm, and to decipher what those messages are telling us about the varied constituent objects in the Universe at present and in th...
متن کاملGeneral properties of astrophysical reaction rates in explosive nucleosynthesis
Fundamental differences in the prediction of reaction rates with intermediate and heavy target nuclei compared to the ones with light nuclei are discussed, with special emphasis on stellar modifications of the rates. Ground and excited state contributions to the stellar rates are quantified, deriving a linear weighting of excited state contributions despite of a Boltzmann population of the nucl...
متن کامل