Calculation of the equation of state of neutron star matter

dc.contributor.advisor	Centelles Aixalà, Mario
dc.contributor.author	Hernández Toledo, Adrià
dc.date.accessioned	2023-07-25T08:34:44Z
dc.date.available	2023-07-25T08:34:44Z
dc.date.issued	2023-06
dc.description	Treballs Finals de Grau de Física, Facultat de Física, Universitat de Barcelona, Curs: 2023, Tutor: Mario Centelles Aixalà	ca
dc.description.abstract	Symmetric nuclear matter, asymmetric nuclear matter and β-stable nuclear matter are discussed and modeled through a Lagrangian density of relativistic mean field (RMF) theory using a σ meson to describe the attractive interaction between nucleons, a ω meson to describe the repulsive interaction and a ρ meson to describe the asymmetry effects with the NL3 parametrization.	ca
dc.format.extent	5 p.
dc.format.mimetype	application/pdf
dc.identifier.uri	https://hdl.handle.net/2445/201118
dc.language.iso	eng	ca
dc.rights	cc-by-nc-nd (c) Hernández, 2023
dc.rights.accessRights	info:eu-repo/semantics/openAccess	ca
dc.rights.uri	http://creativecommons.org/licenses/by-nc-nd/3.0/es/	*
dc.source	Treballs Finals de Grau (TFG) - Física
dc.subject.classification	Equació d'estat	cat
dc.subject.classification	Estels de neutrons	cat
dc.subject.classification	Treballs de fi de grau	cat
dc.subject.other	Equation of state	eng
dc.subject.other	Neutron stars	eng
dc.subject.other	Bachelor's theses	eng
dc.title	Calculation of the equation of state of neutron star matter	eng
dc.type	info:eu-repo/semantics/bachelorThesis	ca

Fitxers

Mostrant 1 - 1 de 1