S-factor

The astrophysical S-factor $S (E)$ is a rescaled variant of the total cross section $σ (E)$ that accounts for the Coulomb repulsion between charged reactants.

Definition

The quantity is defined as[1]

S(E)\equiv {\frac {E}{\exp(-2\pi \eta )}}\sigma (E)

Here, $η$ is the dimensionless Sommerfeld parameter,

\eta \equiv {\frac {Z_{1}Z_{2}e^{2}}{4\pi \epsilon _{0}\hbar v}}

where

$Z 1 Z 2 e 2$ is the product of the charges of the reactants and
$v$ is the magnitude of the relative incident velocity.

Motivation

The Coulomb barrier causes the cross section to have a strong exponential dependence on the center-of-mass energy $E$ . The S-factor remedies this by factoring out the Coulomb component of the cross section.

References

Thompson, Ian J.; Nunes, Filomena M. (2009). Nuclear Reactions for Astrophysics: Principles, Calculations and Applications of Low-Energy Reactions. Cambridge University Press. p. 5. ISBN 978-0-521-85635-5.

This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.

[1] Thompson, Ian J.; Nunes, Filomena M. (2009). Nuclear Reactions for Astrophysics: Principles, Calculations and Applications of Low-Energy Reactions. Cambridge University Press. p. 5. ISBN 978-0-521-85635-5.