Given these particles’ mean lifetime of 880 seconds (10[2])and the time from freeze-out (10[3])to the onset of (10[1])BBNS, (10[1])one can calculate (10[1])an abundance denoted Y. The timescale of these particles’ capture differentiates (10[1])two reactions that occur (10[1])in AGB (-5[1])stars and (10[1])during supernovae, (10[1]-5[1])called the s- and r-processes. (10[2]-5[2])A different particle (10[1]-5[2])decays into one of these (-5[1])particles (10[1]-5[1])in the first (10[1])step (-5[1])of the (10[1]-5[1])p-p chain. (10[1]-5[2])[emphasize] Above the Chandrasekhar (-5[2])(“chun-druh-SHAY-kur”) limit (10[1])but below the (10[3])TOV limit, (10[2])these (10[1]-5[1])particles’ (10[3]-5[2])degeneracy (10[5]-5[4])pressure (10[1]-5[1])keeps (10[1]-5[2])massive (10[2]-5[4])stars (-5[1])from (10[2]-5[1])turning into (10[1])black (10[9]-5[1])holes. (10[1]-5[2])Pulsars (10[1])are (10[1])rapidly (10[1]-5[2])rotating (10[1])members of (10[1])a (-5[1])class of (10[1])extremely dense (10[3])stars made of (10[2])these (10[16])particles. (10[1])For (10[2])10 (10[1])points, name (10[1])these (10[1])subatomic (-5[2])particles with (10[1])no (10[6])charge. (10[35]0[2])■END■