A model for rp-process within the (p, γ)-(γ, p) equilibrium approximation and its application

Many of the stable nuclei at the neutron-deficient side of the beta-stability valley cannot be synthesized in the neutron-capture processes. The origin of the so-called p-nuclei has been a long standing question in the nuclear astrophysics. The rapid-proton capture process (rp-process) proposed in the 1980s was one of the possible mechanisms to be responsible for some light p-nuclei. In this work, a model for rapid-proton capture process (rp-process), within the (p, γ)-(γ, p) equilibrium approximation, is established. In the framework of this model, the influence of astrophysical conditions (i.e., proton number density, temperature, and proton irradiation time) on the rp-abundance pattern is investigated. In addition, the recent-measured mass data of neutron-deficient atomic nuclei by using the storage ring mass spectrometry at IMP, Lanzhou, are employed in our calculation. It is found that the abundance at A = 41 is increased by two orders of magnitude when using the new by determined mass of ⁴¹Ti, while the uncertainty of the computed abundance is reduced by almost two orders of magnitude.