Investigation of the triple-alpha reaction in a full three-body approach

Abstract

Background: The triple-alpha reaction is the key to our understanding about the nucleosynthesis and the observed abundance of ${}^{12}$C in stars. The theory of this process is well established at high temperatures but rather ambiguous in the low temperature regime where measurements are impossible. Purpose: Develop a new three-body method, which tackles properly the scattering boundary condition for three charged particles and takes into account both the resonant and the non-resonant reaction mechanisms on the same footing, to compute the triple-alpha reaction rate at low temperatures. Methods: We combine the R-matrix expansion, the R-matrix propagation method, and the screening technique in the hyperspherical harmonics basis. Results: Both the $2_1^{+}$ bound state and the $0_2^{+}$ resonant state in ${}^{12}$C are well reproduced. We also study the cluster structure of these states. We calculate the triple-alpha reaction rate for $\mathrm{T}=0.01-0.1$ GK. Conclusions: We obtain the same rate as NACRE for temperatures above 0.07 GK, but the new rate is largely enhanced at lower temperatures ($\approx 10^{12}$ at 0.02 GK). The differences are caused by the direct capture contribution to the reaction when three alpha particles can not reach the resonant energies.