English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

In this paper we analyze the nuclear fusion rate between equal nuclei for allfive different nuclear burning regimes in dense matter (two thermonuclearregimes, two pycnonuclear ones, and the intermediate regime). The rate isdetermined by Coulomb barrier penetration in dense environments and by theastrophysical S-factor at low energies. We evaluate previous studies of theCoulomb barrier problem and propose a simple phenomenological formula for thereaction rate which covers all cases. The parameters of this formula can bevaried, taking into account current theoretical uncertainties in the reactionrate. The results are illustrated for the example of the ^{12}C+^{12}C fusionreaction. This reaction is very important for the understanding of nuclearburning in evolved stars, in exploding white dwarfs producing type Iasupernovae, and in accreting neutron stars. The S-factor at stellar energiesdepends on a reliable fit and extrapolation of the experimental data. Wecalculate the energy dependence of the S-factor using a recently developedparameter-free model for the nuclear interaction, taking into account theeffects of the Pauli nonlocality. For illustration, we analyze the efficiencyof carbon burning in a wide range of densities and temperatures of stellarmatter with the emphasis on carbon ignition at densities rho > 10^9 g/cc.Comment: 22 pages, 6 figures, accepted for publication in PR

Nuclear fusion in dense matter: Reaction rate and carbon burning