Equation of state of nuclear matter with applications to rapid rotating neutron stars
Abstract
Neutron stars manifest one of the Universe's densest objects, where matter is compressed at high densities, and nuclear physics combines with general relativity. The dense nuclear matter is described by the yet unknown equation of state, simulating the fluid interior, where its combination with the Tolman-Oppenheimer-Volkoff equations provides the neutron star structure. Although cold non-rotating neutron stars are a valuable source of constraints, temperature, and high rotational frequencies will significantly improve and extend our knowledge. In particular, the research is focused on the construction of both cold and hot, lepton-rich matter equations of state and their implications on macroscopic as well as microscopic quantities of neutron stars. Specifically, universal relations are produced for each representative case, and a criterion for the final fate of compact objects is extracted. Furthermore, the research is extended to proto-neutron stars and the hot and rapidly rotating r ...
show more
![]() | |
![]() | Download full text in PDF format (4.33 MB)
(Available only to registered users)
|
All items in National Archive of Phd theses are protected by copyright.
|
Usage statistics

VIEWS
Concern the unique Ph.D. Thesis' views for the period 07/2018 - 07/2023.
Source: Google Analytics.
Source: Google Analytics.

ONLINE READER
Concern the online reader's opening for the period 07/2018 - 07/2023.
Source: Google Analytics.
Source: Google Analytics.

DOWNLOADS
Concern all downloads of this Ph.D. Thesis' digital file.
Source: National Archive of Ph.D. Theses.
Source: National Archive of Ph.D. Theses.

USERS
Concern all registered users of National Archive of Ph.D. Theses who have interacted with this Ph.D. Thesis. Mostly, it concerns downloads.
Source: National Archive of Ph.D. Theses.
Source: National Archive of Ph.D. Theses.