NUCLEAR PHYSICS: Determination of the stellar reaction rate for 12C(α, γ)16O: using a new expression with the reaction mechanism

Details NUCLEAR PHYSICS: Determination of the stellar reaction rate for 12C(α, γ)16O: using a new expression with the reaction mechanism NUCLEAR PHYSICS: Determination of the stellar reaction rate for 12C(α, γ)16O: using a new expression with the reaction mechanism

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009chphb..18.1421x&link_type=abstract

Chinese Physics B, Volume 18, Issue 4, pp. 1421-1427 (2009).

Physics

Scientific paper

The astrophysical reaction rate of 12C(α, γ)16O plays a key role in massive star evolution. However, this reaction rate and its uncertainties have not been well determined yet, especially at T9 = 0.2. The existing results even disagree with each other to a certain extent. In this paper, the E1, E2 and total (E1+E2) 12C(α, γ)16O reaction rates are calculated in the temperature range from T9 = 0.3 to 2 according to all the available cross section data. A new analytic expression of the 12C(α, γ)16O reaction rate is brought forward based on the reaction mechanism. In this expression, each part embodies the underlying physics of the reaction. Unlike previous works, some physical parameters are chosen from experimental results directly, instead of all the parameters obtained from fitting. These parameters in the new expression, with their 3σ fit errors, are obtained from fit to our calculated reaction rate from T9 = 0.3 to 2. Using the fit results, the analytic expression of 12C(α, γ)16O reaction rate is extrapolated down to T9 = 0.05 based on the underlying physics. The 12C(α, γ)16O reaction rate at T9 = 0.2 is (8.78 ± 1.52) × 1015 cm's-1 mol-1. Some comparisons and discussions about our new 12C(α, γ)16O reaction rate are presented, and the contributions of the reaction rate correspond to the different part of reaction mechanism are given. The agreements of the reaction rate below T9 = 2 between our results and previous works indicate that our results are reliable, and they could be included in the astrophysical reaction rate network. Furthermore, we believe our method to investigate the 12C(α, γ)16O reaction rate is reasonable, and this method can also be employed to study the reaction rate of other astrophysical reactions. Finally, a new constraint of the supernovae production factor of some isotopes are illustrated according to our 12C(α, γ)16O reaction rates.

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