Hydrogen burning of 20Ne and 22Ne in stars

Details Hydrogen burning of 20Ne and 22Ne in stars Hydrogen burning of 20Ne and 22Ne in stars

Apr 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975nupha.241..460r&link_type=abstract

Nuclear Physics A, Volume 241, Issue 3, p. 460-486.

Physics

Nuclear Physics

25

Nuclear Reactions

Scientific paper

The 20Ne(p, γ)21Na capture reaction has been studied in the energy range Ep = 0.37-2.10 MeV. Direct-capture transitions to the 332 (5/2+) and 2425 keV (1/2+) states have been found with spectroscopic factors of C2S(1d) = 0.77+/-0.13 and C2S(2s) = 0.90+/-0.12, respectively. The high-energy tail of the 2425 keV state, bound by 7 keV against proton decay, has also been observed in the above energy range as a subthreshold resonance. The excitation function for this tail is consistent with a single-level Breit-Wigner shape for a γ-width of Γγ = 0.31+/-0.07 eV at Ex = 2425 keV. The extrapolation of these data to stellar energies gives an astrophysical S-factor of S(0) = 3500 keV . b. Two new resonances at Ep = 384+/-5 and 417+/- 5 keV have been observed with strengths of ωγ = 0.11+/-0.02 and 0.06+/-0.01 meV, corresponding to the known states at Ex(Jπ) = 2798 (1/2-) and 2829 keV (presumably 9/2+), respectively. For the known Ep = 1830 keV resonance, a strength of ωγ = 1.0+/- 0.3 eV and a total width of Γ = 180+/- 15 keV were found. Branching ratios as well as transition strengths have been obtained for these three states. The Q-value for the 20Ne(p, γ)21Na reaction (Q = 2432.3 +/- 0.5 keV) as well as excitation energies for many low-lying states in 21Na have been measured. No evidence was found for the existence of the state reported at Ex = 4308+/-4 keV.
In the case of 22Ne(p, γ)23Na, direct-capture transitions to six final bound states have been observed revealing sizeable spectroscopic factors for these states. The astrophysical S-factor extrapolated from these data to stellar energies, is S(0) = 67 +/- 12 keV . b.
The astrophysical as well as the nuclear structure aspects of the present results are discussed.

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