Thermodynamics and Quantum Properties of Ultra-Relativistic Degenerate Electron Gas in White Dwarf and Neutron Stars
| dc.contributor.advisor | Elfagd, Yitagesu (PhD) | |
| dc.contributor.author | Ali, Ibrahim | |
| dc.date.accessioned | 2022-03-15T11:25:27Z | |
| dc.date.accessioned | 2023-11-09T11:26:51Z | |
| dc.date.available | 2022-03-15T11:25:27Z | |
| dc.date.available | 2023-11-09T11:26:51Z | |
| dc.date.issued | 2022-01-07 | |
| dc.description.abstract | We study the problem of the relativistic free electron gas at arbitrary degenerate electron gas. The speci_c heat at constant volume and particle number cv and the speci_c heat at constant pressure and particle number cp are calculated. The equation of state is also studied. Non degenerate and degenerate electron limits are considered. We generalize the formulas obtained in the non-relativistic and ultra-relativistic degenerate electron gas. Neutron stars are much denser than white dwarf stars, which, once again, causes the core of the stars to collapse. The compression of neutrons in the contracting core, however, creates a neutron degenerate pressure. This pressure, analogous to the electron degenerate pressure in white dwarf stars, combats the gravitational collapse of the star. If, however, the neutron star is too massive (more than three solar masses), the neutron degenerate pressure fails and the neutron star collapses into a black hole. We now see that the role of both the neutron degenerate pressure, and the electron degenerate pressure is crucial to the maintained stability of a star The energy corresponding to this momentum, called the Fermi energy which we will discuss in the next section will also increase. So, with a decreasing volume and an increasing particle momentum, we can say that a pressure formed inside of the core of the star, and continues to increase as long as the volume continues to increase, and that there are degenerate neutron energy states. Now that we know where the pressure comes from, we can _nally derive a mathematical expression for the neutron degeneracy pressure by non-relativistic neutrons inside of a neutron star. | en_US |
| dc.identifier.uri | http://10.90.10.223:4000/handle/123456789/30612 | |
| dc.language.iso | en | en_US |
| dc.publisher | Addis Ababa University | en_US |
| dc.subject | Thermodynamics | en_US |
| dc.subject | Quantum Properties | en_US |
| dc.subject | Ultra-Relativistic | en_US |
| dc.subject | Degenerate Electron | en_US |
| dc.subject | Gas in White Dwarf | en_US |
| dc.subject | Neutron Stars | en_US |
| dc.title | Thermodynamics and Quantum Properties of Ultra-Relativistic Degenerate Electron Gas in White Dwarf and Neutron Stars | en_US |
| dc.type | Thesis | en_US |