𝑅-Process Nucleosynthesis in MHD Jet Explosions of Core-Collapse Supernovae

Figure 1

(a) It shows the evolution of the neutrino luminosity after the collapse for a model 1. (b) It shows changes in electron fraction (𝑌_𝑒) when the central density becomes 10¹², 10¹³, and 10¹⁴ g cm⁻³, respectively, and neutrino fraction (𝑌_𝜈) when the central density becomes 10¹³ and 10¹⁴ g cm⁻³, respectively. Our results could approximate those of Liebendörfer et al. [31].

(a)

(b)