The path to improved reaction rates for astrophysics

  title={The path to improved reaction rates for astrophysics},
  author={Thomas Rauscher},
  journal={International Journal of Modern Physics E-nuclear Physics},
  • T. Rauscher
  • Published 20 October 2010
  • Physics
  • International Journal of Modern Physics E-nuclear Physics
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 present the basic definitions essential for studies in nuclear astrophysics, to point out the differences between nuclear reactions taking place in stars and in a terrestrial laboratory, and to illustrate some of the challenges to be faced in theoretical and experimental studies of those reactions. The… 
General 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
Sensitivity of Astrophysical Reaction Rates to Nuclear Uncertainties
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
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
Theory Considerations For Nucleosynthesis Beyond Fe With Special Emphasis On p-Nuclei In Massive Stars
Nucleosynthesis of heavy elements requires the use of different experimental and theoretical methods to determine astrophysical reaction rates than light element nucleosynthesis. Additionally, there
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
Radiation signatures of nuclear reactions in very hot astrophysical plasmas
The importance of nuclear reactions in low-density astrophysical plasmas with ion temperatures kT>1 MeV has been recognized for more than thirty years. However, the lack of comprehensive data banks
The vp-process: critical nuclear physics and astrophysical implications
The neutrino-p-process is thought to occur in the innermost proton-rich layers ejected in core-collapse supernovae. The importance of the vp-process lies in the fact that it may contribute to the
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
Cross section of α -induced reactions on Au197 at sub-Coulomb energies
Statistical model calculations have to be used for the determination of reaction rates in large-scale reaction networks for heavy-element nucleosynthesis. A basic ingredient of such a calculation is
EMPIRE: A code for nuclear astrophysics
The nuclear reaction code EMPIRE is presented as a useful tool for nuclear astrophysics. EMPIRE combines a variety of the reaction models with a comprehensive library of input parameters providing a


Differences between stellar and laboratory reaction cross sections
Nuclear reactions proceed differently in stellar plasmas than in the laboratory due to the thermal effects in the plasma. On one hand, a target nucleus is bombarded by projectiles distributed in
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
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.
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
Nuclei in the Cosmos
This white paper, directed to the Stars and Stellar Evolution panel, has three objectives: 1) to provide the Astro2010 Decadal Survey with a vista into the goals of the nuclear physics and nuclear