Given these particles’ mean lifetime of 880 seconds (10[1])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 (-5[1])stars and during supernovae, called the s- and r-processes. A different particle decays into one of these particles (-5[1])in the first (10[1])step (-5[1])of the (-5[1])p-p chain. [emphasize] Above the Chandrasekhar (“chun-druh-SHAY-kur”) limit but below the TOV limit, these particles’ (10[1])degeneracy pressure keeps massive stars from turning into black (10[1])holes. Pulsars are rapidly rotating members of a class of extremely dense (10[1])stars made of these (10[1])particles. (10[1])For 10 points, name these (10[1])subatomic particles with no charge. (10[3])■END■