Given these particles’ mean lifetime of 880 seconds and the time from freeze-out to the onset of BBNS, one can calculate an abundance denoted Y. The timescale of these particles’ capture differentiates two reactions that occur in AGB stars and during supernovae, called the s- and r-processes. (-5[1])A different particle decays into one of these particles in the first step of the p-p chain. [emphasize] Above the Chandrasekhar (“chun-druh-SHAY-kur”) limit but below the (10[1])TOV limit, these particles’ degeneracy (-5[2])pressure keeps massive (-5[2])stars from turning into black holes. Pulsars are rapidly (-5[1])rotating (10[1])members of a class of (10[1])extremely dense stars made of these (10[2])particles. For 10 (10[1])points, name these subatomic particles with no (10[2])charge. (10[4])■END■