3.(a) Using for kinetic and gravitational energies of the white dwarf star simplified ex pression...
Stars much heavier than our sun will not form white dwarf, but collapse further, becoming (if condition are right) neutron stars. They result from the supernova explosion of a massive star, combined with gravitational collapse, that compresses the core past white dwarf star density to that of atomic nuclei. Eventually neutron degeneracy pressure stabilizes the collapse, just as the electron does for white dwarfs. The Fermi Energy is given by where Z/A =1 and V corresponds to volume. The neutron...
2) Densities We discussed White Dwarfs and Neutron stars, very dense objects compared to stars like our sun. On the other hand, we also discussed Red Giants which are much less dense than our sun. To realize just how dense, please compute the average densities (in kg/m) for a) the sun (Rsun=7 x 10 km, Msun= 2 x 1030 kg) b) when the sun becomes a red giant (R= 1AU, M=Msun). By what factor is a Red Giant less dense...
If a neutron star and a white dwarf has a total mass of 1M. If the white dwarf has a radius of 9 x 106 m and the neutron star has a radius of 11 km. i) Compare the surface gravity of both stars. ii) What is the density of the neutron star? iii) Assuming the neutron star is entirely made up of neutrons, and that the interparticle separation of a gas of density n is l = n-1/3. How...
3 GM2 (5) The gravitational potential of a uniform-density sphere of mass M and radius R is E,-- Consider a white dwarf star which contains N electrons whose Fermi energy is Es. Since kaT <<Ef, the average electron energy is 3/5Er (derived in assignment 1) and the total electron energy is Ed-3/5NEs. The energies of the nuclei can be neglected. OE (a) Derive an expression for the gravitational pressure: P- OE (b) Derive an expression for the degeneracy pressure: Pa-...