1) Problem 3 from Chapter 2 of Ashcroft & Mermin.
(a) Given M0 = 2 x 1033 g for the mass of the Sun, estimate the number of electrons in the Sun. In a white dwarf star this number of electrons may be ionized and contained in a sphere of radius 2 x 109 cm; find the Fermi energy of the electrons in electron volts.
(b) The energy of an electron in the relativistic
limit
is related to the wave vector as
.
Show that the Fermi energy, in this limit, is
.
(c) If the above number of electrons
were contained within a pulsar of radius 10 km, show that the Fermi
energy would be ~108 eV.
p +
e- is only 0.8 X 106 eV, which is not large enough to enable
many electrons to form a Fermi sea. The neutron decay proceeds only
until the electron concentration builds up enough to create a Fermi level of
0.8 X 106 eV, at which point the neutron, proton, and electron
concentrations are in equilibrium.