Astrophysical reaction rates from statistical model calculations

By T. Rauscher, Friedrich-Karl Thielemann. 2000

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Theoretical reaction rates in the temperature range 0.01 x 10(9) less than or equal to T(K) less than or equal to 10.0 x 10(9) are calculated in the statistical model (Hauser-Feshbach formalism) for targets with 10 less than or equal to Z less than or equal to 83 (Ne to Bi) and for a mass range reaching the neutron and proton driplines. Reactions considered are (n, gamma), (n, p), (n, alpha), (p, gamma), (p, alpha), (alpha, gamma), and their inverse reactions. Reaction rates as a function of temperature for thermally populated targets are given by seven analytical parameter fits. To facilitate comparison with experimental rates, the stellar enhancement factors are also tabulated. Two complete sets of rates have been calculated, one of which includes a phenomenological treatment of shell quenching for neutron-rich nuclei. These extensive datasets are provided on-line as electronic files, while a selected subset from one calculation is given as printed tables. A summary of the theoretical inputs and advice on the use of the provided tabulations is included. (C) 2000 Academic Press.

Subfields: Aerospace Engineering, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5a4de4e4e583f44bda36276c7a701301814c6ea0

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Citations in the corpus

Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r‐process nuclei (2010, methodology): “The neutron capture rates for nuclei with Z 6 83 are obtained from the work of Rauscher & Thielemann (2000) and are based on two different nuclear mass models: the Finite Range Droplet Model (Möller et al. 1995) and the Quenched version of the Extended Thomas Fermi with Strutinsky Integral model…”
Violent mergers of nearly equal-mass white dwarf as progenitors of subluminous Type Ia supernovae (2011, methodology): “The nuclear reaction rates are taken from the latest (2009) release of the REACLIB database (Rauscher & Thielemann 2000).”
Impact of ejecta morphology and composition on the electromagnetic signatures of neutron star mergers (2017, methodology): “The reaction rates are from the compilation of Rauscher & Thielemann (2000) for the finite range droplet model (FRDM; Möller et al. 1995) and the weak interaction rates (e−e+-captures and β-decays) are the same as used in Arcones & Martínez-Pinedo (2011).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, methodology): “As a test, we repeat all the nucleosynthesis calculations of model ST with the theoretical rates (Aikawa et al. 2005) replaced by those of Rauscher & Thielemann (2000).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, methodology): “The majority of reaction and decay rates have been taken from a compilation of REACLIB database (Rauscher & Thielemann 2000) and its extension, JINA REACLIB 3 (Cyburt et al. 2010), in which theoretical ones are mainly on the basis of FRDM. Physical uncertainties of β-decay half-lives and effects of…”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, methodology): “For neutron capture rates not included in KADoNIS, we adopt data from the Basel REACLIB database, revision 20090121 (Rauscher & Thielemann 2000).”
Nucleosynthesis in the Early Galaxy (2007, methodology): “The nuclear reaction rates were taken from the recent REACLIB compilation, which includes theoretical reaction rates based on NON-SMOKER statistical model calculations (Rauscher & Thielemann 2000) with Q-values obtained with the FRDM (Möller et al. 1995) mass model.”
CHARGED-PARTICLE AND NEUTRON-CAPTURE PROCESSES IN THE HIGH-ENTROPY WIND OF CORE-COLLAPSE SUPERNOVAE (2010, methodology): “For these purposes both the rate sets based on FRDM and ETFSI-Q of Rauscher & Thielemann (2000) were used for the experimentally unknown rates of neutron-rich nuclei.”
Turbulent Convection in Stellar Interiors. I. Hydrodynamic Simulation (2006, methodology): “The reaction rates, including 12C(α, γ)16O, are from Rauscher & Thielemann (2000).”
Models for Type I X-Ray Bursts with Improved Nuclear Physics (2003, methodology): “All other reaction rates were calculated using the Hauser-Feshbach code Non-Smoker as described by Rauscher & Thielemann (2000).”
Non-standard s process in low metallicity massive rotating stars (2011, methodology): “We used the reaction library (REACLIB) from Rauscher & Thielemann (2000), but with major updates.”
The s process: Nuclear physics, stellar models, and observations (2010, methodology): “…experimental cross section information, recommended values were derived from calculations with the Hauser-Feshbach statistical model code NON-SMOKER (Rauscher and Thielemann, 2000), which were 13 empirically corrected for known systematic deficiencies in the nuclear input of the calculation.”
NEUTRINO-DRIVEN WINDS IN THE AFTERMATH OF A NEUTRON STAR MERGER: NUCLEOSYNTHESIS AND ELECTROMAGNETIC TRANSIENTS (2015, methodology): “Our calculations are based on the FRDM mass model (Möller et al. 1995) and consistently calculated nuclear reaction rates (Rauscher & Thielemann 2000).”
The Intermediate r-process in Core-collapse Supernovae Driven by the Magneto-rotational Instability (2016, methodology): “We perform nucleosynthesis calculation using a nuclear reaction network code (Nishimura et al. 2015, 2016), with reaction rate data taken mostly from Rauscher & Thielemann (2000).”