Unit:
Κατεύθυνση Πυρηνική Φυσική και Φυσική Στοιχειωδών Σωματιδίων (ΒΑΣΙΚΗ ΦΥΣΙΚΗ)Library of the School of Science
Supervisors info:
Φ. Διάκονος, Αναπληρωτής Καθηγητής, Τμήμα Φυσικής, ΕΚΠΑ
Π. Παπακωνσταντίνου, Ερευνήτρια, IBS, Daejeon
Θ. Μερτζιμέκης, Αναπληρωτής Καθηγητής, Τμήμα Φυσικής, ΕΚΠΑ
Original Title:
Συναρτησοειδές ενεργειακής πυκνότητας KIDS και σχέση μάζας-ακτίνας αστέρων νετρονίων
Translated title:
KIDS energy density functional and mass - radius relation of neutron stars
Summary:
The efforts to understand neutron stars continue with intense interest, as it has been confirmed that it is also during the merging of two neutron stars that r-process takes place. Many efforts are made to determine the nuclear equation of state which governs the properties and evolution of neutron stars. Especially important is to constrain the parameters of the nuclear symmetry energy. In those efforts, nuclear energy density functional (EDF) theory has been a very useful tool, as it encodes efficiently correlations and the three-body force and it provides a unified framework for the description both of nuclei, which can be studied on Earth, and of infinite matter and its nuclear equation of state, which is a necessary input in order to find the mass - radius relation of neutron stars.
In the present study, a new nuclear EDF, the KIDS functional, is explored with a focus on the nuclear symmetry energy. In particular, the form of the functional allows us to examine how the maximum possible mass of a neutron star is affected by the choice of high-order derivatives of the symmetry energy, which are not well constrained from nuclear data and observations. Some first constraints on the skewness are presented, which will help guide further refinements.
Main subject category:
Science
Keywords:
Theoretical Nuclear Physics, Nuclear Energy Density Functionals, Neutron Stars, KIDS Functional, Symmetry Energy, Equations of State
