author={Thomas Rauscher},
  journal={The Astrophysical Journal Supplement Series},
  • T. Rauscher
  • Published 3 May 2012
  • Physics, Chemistry
  • The Astrophysical Journal Supplement Series
Sensitivities of nuclear reaction rates to a variation of nuclear properties are studied. Target nuclei range from proton- to neutron dripline for 10 ⩽ Z ⩽ 83. Reactions considered are nucleon- and α-induced reactions mediated by strong interaction. The contribution of reactions occurring on the target ground state to the total stellar rate is also given. General dependencies on various input quantities are discussed. Additionally, sensitivities of laboratory cross-sections of nucleon-, α-, and… 
Abundance Uncertainties Obtained With the PizBuin Framework For Monte Carlo Reaction Rate Variations
Uncertainties in nucleosynthesis models originating from uncertainties in astrophysical reaction rates were estimated in a Monte Carlo variation procedure. Thousands of rates were simultaneously
Sensitivity to neutron captures and β-decays of the enhanced s-process in rotating massive stars at low metallicities
The s-process in massive stars, producing nuclei up to A ≈ 90, has a different behaviour at low metallicity if stellar rotation is significant. This enhanced s-process is distinct from the s-process
Uncertainties in s-process nucleosynthesis in massive stars determined by Monte Carlo variations
The s-process in massive stars produces the weak component of the s-process (nuclei up to A ∼ 90), in amounts that match solar abundances. For heavier isotopes, such as barium, production through
Challenges in nucleosynthesis of trans-iron elements
Nucleosynthesis beyond Fe poses additional challenges not encountered when studying astrophysical processes involving light nuclei. Astrophysical sites and conditions are not well known for some of
Measurement of (α,n) reaction crosssections of erbium isotopes for testingastrophysical rate predictions
The γ-process in core-collapse and/or type Ia supernova explosions is thought to explain the origin of the majority of the so-called p nuclei (the 35 protonrich isotopes between Se and Hg).
Nuclear physics uncertainties of the astrophysical gamma-process studied through the 64Zn(p,alpha)61Cu and 64Zn(p,gamma)65Ga reactions
In a recent work, the cross section measurement of the 64Zn(p,α)61Cu reaction was used to prove that the standard α-nucleus optical potentials used in astrophysical network calculation fail to
Uncertainties in νp-process nucleosynthesis from Monte Carlo variation of reaction rates
It has been suggested that a νp-process can occur when hot, dense, and proton-rich matter is expanding within a strong flux of antineutrinos. In such an environment, proton-rich nuclides can be
Impacts of nuclear-physics uncertainty in stellar temperatures on the s-process nucleosynthesis
N. Nishimura, G. Cescutti, R. Hirschi, T. Rauscher, J. Den Hartogh, and A. St J. Murphy, 'Impacts of nuclear-physics uncertainty in stellar temperatures on the s-process nucleosynthesis', in
Revision of the derivation of stellar rates from experiment and impact on Eu s-process contributions
A new, general formalism to include experimental data in revised stellar rates is discussed, containing revised uncertainties. Application to the s-process shows that the actual uncertainties in the
Correlated energy uncertainties in reaction rate calculations
Context. Monte Carlo methods can be used to evaluate the uncertainty of a reaction rate that arises from many uncertain nuclear inputs. However, until now no attempt has been made to find the effect


The path to improved reaction rates for astrophysics
This review focuses on nuclear reactions in astrophysics and, more specifically, on reac- tions with light ions (nucleons andparticles) proceeding via the strong interaction. It is intended to
Nuclear inputs for nucleosynthesis applications
Although an important effort has been devoted in the last decades to measure reaction cross sections of interest in astrophysics, most nuclear astrophysics applications still require the use of
Modern models of s-process nucleosynthesis in stars require stellar reaction rates of high precision. Most neutron-capture cross-sections in the s-process have been measured, and for an increasing
Charged particle reaction cross sections and nucleosynthesis.
Suppression of the stellar enhancement factor and the reaction 85Rb(p,n)85Sr
Astrophysical reaction rates are central to tracing changes in the abundances of nuclei by nuclear reactions. They provide the temperature- and density-dependent coefficients entering reaction
Alpha-induced reaction cross section measurements on $^{151}$Eu for the astrophysical $\gamma$-process
In order to extend the experimental database relevant for the astrophysical -process towards the unexplored heavier mass region, the cross sections of the 151 Eu(�,) 155 Tb and 151 Eu(�,n) 154 Tb
Coulomb suppression of the stellar enhancement factor.
It is shown that the stellar effects can be minimized in the charged particle channel, even when the reaction Q value is negative, which confirms a previously derived modification of a global optical proton potential.
Investigation of alpha-induced reactions on 130Ba and 132Ba and their importance for the synthesis of heavy p nuclei
Captures of alpha particles on the proton-richest Barium isotope, 130Ba, have been studied in order to provide cross section data for the modeling of the astrophysical gamma process. The cross