Relevant energy ranges for astrophysical reaction rates

  title={Relevant energy ranges for astrophysical reaction rates},
  author={Thomas Rauscher},
  journal={Physical Review C},
  • T. Rauscher
  • Published 14 March 2010
  • Physics
  • Physical Review C
Effective energy windows (Gamow windows) of astrophysical reaction rates for (p,gamma), (p,n), (p,alpha), (alpha,gamma), (alpha,n), (alpha,p), (n,gamma), (n,p), and (n,alpha) on targets with 10 >= Z >= 83 from proton to neutron dripline are calculated using theoretical cross sections. It is shown that widely used approximation formulas for the relevant energy ranges are not valid for a large number of reactions relevant to hydrostatic and explosive nucleosynthesis. The influence of the energy… 

Theoretical cross section calculation of the 112Sn(α,γ)116Te reaction for the astrophysical P process

The theoretical cross section calculations for the astrophysical p process are very crucial due to the most of the related reactions are technically very difficult to measure at the laboratory. On


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

Cross sections of low energy (p,γ) and (p,n)-reactions on selenium isotopes for the astrophysical γ-process

The cross sections of the proton radiative captures Se(p, γ)Br, Se(p, γ)Br, and Se(p, γ)Br as well as the threshold Se(p, n)Br and Se(p, n)Br reactions have been measured in the astrophysical

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

Successful Prediction of Total α-Induced Reaction Cross Sections at Astrophysically Relevant Sub-Coulomb Energies Using a Novel Approach.

A simple barrier transmission model is suggested and it is shown that this simple model in combination with a well-chosen α-nucleus potential is able to predict total α-induced reaction cross sections for a wide range of heavy target nuclei above A≳150 with uncertainties below a factor of 2.

The Feasibility of Studying 44Ti(α, p)47V Reaction at Astrophysical Energies

The gamma-ray lines from the decay of 44Ti have been observed by space-based gamma-ray telescopes from two supernova remnants. It is believed that the 44Ti(α, p)47V reaction dominates the destruction

Systematic Study Of (p,γ) Reactions On Ni Isotopes

A systematic study of the radiative proton capture reaction for all stable nickel isotopes is presented. The results were obtained using 2.0–6.0 MeV protons from the 11-MV tandem Van de Graaff

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

Investigation of reactions relevant for the γ process using in-beam γ-ray spectroscopy

The reaction 89Y(p, γ)90Zr was studied at five proton energies close to the Gamow window. This reaction is of astrophysical importance, since it is located in a mass region, where the p-nuclei



Nuclear physics of stars

Preface. 1 Aspects of Nuclear Physics and Astrophysics. 1.1 History. 1.2 Nomenclature. 1.3 Solar System Abundances. 1.4 Astrophysical Aspects. 1.4.1 General Considerations. 1.4.2 Hertzsprung-Russell

Cauldrons in the cosmos

See EPAPS Document No. [number will be inserted by publisher] at [URL] for a ASCII file containing the full table of energy windows and shifts. For more information on EPAPS

    Phys. Rev. C

    • Phys. Rev. C
    • 2007

    Atomic Data Nucl. Data Tables

    • 2001

    Thielemann , Atomic Data Nucl

    • Data Tables
    • 2006


    • J. Suppl. 18, 247
    • 1969