Tables of thermonuclear reaction rates for low-mass nuclei (1 ⩽ Z ⩽ 14)

  title={Tables of thermonuclear reaction rates for low-mass nuclei (1 ⩽ Z ⩽ 14)},
  author={Georgeanne R. Caughlan and William A. Fowler and Michael J. Harris and Barbara A. Zimmerman},
  journal={Atomic Data and Nuclear Data Tables},
Astrophysical Reaction Rate of 12C(α, γ)16O
A new astrophysical reaction rate of 12C(α, γ)16O has been calculated based on our recent determination of the E1- and E2-capture cross sections. The R-matrix method has been applied to describe the
New Stellar Reaction Rate for 12C(α, γ)16O
The 12C(α, γ)16O reaction rate has been reevaluated using recently published cross section estimates. The results suggest that the temperature dependence of the reaction rate as given by Caughlan &
An explanation for the solar neutrino problem
A new mechanism of thermonuclear reaction is briefly introduced. It shows that a certain amount of thermonuclear reaction can take place in dense, low-temperature (T < 1 × 105K) plasmas. At a
Influence of two updated nuclear reaction rates on the evolution of low and intermediate mass stars
Two key reactions of hydrostatic nuclear burning in stars have recently been revised by new experimental data - the 14 N(p, γ) 15 O and 3α reaction rates. We investigate how much the new rates
New analytic representation of the thermonuclear reaction rates
  • A. A. Mavrin
  • Chemistry
    Plasma Physics and Controlled Fusion
  • 2018
In the current note, new analytic representations of the Maxwellian reactivities for D(d, n)3He, D(d, p)T, D(3He, p)4He and D(t, n)4He reactions are obtained using a semi-empirical approach. These
The Reaction Rate Sensitivity of Nucleosynthesis in Type II Supernovae
We explore the sensitivity of the nucleosynthesis of intermediate-mass elements (28 ≤ A ≲ 80) in supernovae derived from massive stars to the nuclear reaction rates employed in the model. Two


Thermonuclear Reaction Rates, III
A revision and updating of charged particle reactions involving nuclei with A less than or approximately equal to 30, except for the $sup 2$H(d,$gamma$)$sup 4$He reaction whose reaction rate is very
Stellar weak interaction rates for intermediate mass nuclei. III. Rate tables for the free nucleons and nuclei with A = 21 TO A = 60
Stellar electron and positron emission rates and continuum electron and positron capture rates, as well as the associated neutrino energy loss rates, are tabulated for the free nucleons and 226
Stellar weak-interaction rates for sd-shell nuclei. I - Nuclear matrix element systematics with application to Al-26 and selected nuclei of importance to the supernova problem
Astrophysical positron emission, continuum electron capture, and neutrino energy loss rates are calculated for 26 A1—> 26 Mg, 30 P—» 30 Si, 31 S—> 31 P, 32 S—> 32 P, 33 S-> 33 P, and 35 C1-* 35 S.
Stellar weak interaction rates for intermediate-mass nuclei. II. A = 21 to A = 60
Astrophysical electron and positron emission, continuum electron and positron capture rates, as well as the associated neutrino energy loss rates are calculated for free nucleons and 226 nuclei with
Measurement of the Be-7 (p, gamma) B-8 Reaction Cross Section at Low Energies
The absolute total cross section for the reaction /sup 7/Be ..gamma..)/sup 8/B has been measured for E/sub c.m./ = 117--1230 keV by detecting the delayed ..cap alpha.. particles following the /sup
Neutrino processes and pair formation in massive stars and supernovae.
Abstract : The paper traces the physical properties of matter inside highly evolved stars, on the assumption that the whole material of the star is non-degenerate and that the star is in