A.) estimate the neutron degeneracy pressure (in n/m 2 ) at the center of a 1.4 m ⊙ neutron star. take the central density to be 1.5×10 18 kg/m 3 . use the equations we derived for the speed of electrons to determine if using the formula we derived for the degenerate electron pressure can be used (albeit by replacing m e with m n .) you can also assume for a neutron star that the ratio z/a becomes unity (obviously, yes? ) for a neutron star core.
(b.) compare this pressure with the estimated pressure at the core of the white dwarf, sirius b.