Please use this identifier to cite or link to this item: https://hdl.handle.net/2445/222353
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dc.contributor.advisorManrique Oliva, Alberto-
dc.contributor.authorAlbert Clotet, Aleix-
dc.date.accessioned2025-07-18T07:06:31Z-
dc.date.available2025-07-18T07:06:31Z-
dc.date.issued2025-06-
dc.identifier.urihttps://hdl.handle.net/2445/222353-
dc.descriptionTreballs Finals de Grau de Física, Facultat de Física, Universitat de Barcelona, Curs: 2025, Tutor: Alberto Manrique Olivaca
dc.description.abstractThis project explores the physics of radiative cooling in a cosmological context, focusing on the connection between cooling efficiency and halo mass. We begin by reviewing the main cooling mechanisms and their impact in the cooling function Λ(Z, T). Then, we derive the analytical expressions for the cooling time tcool, highlighting its dependence on gas density and radius. Finally, we implement a numerical code in Fortran to estimate the cooling radius for halos in the range 108.6 − 1015 M⊙ masses. Additionally, we compute the cooling time as a function of radius for a fixed halo mass. These results allow us to identify the regions where gas can effectively cool and potentially form stars.ca
dc.format.extent6 p.-
dc.format.mimetypeapplication/pdf-
dc.language.isoengca
dc.rightscc-by-nc-nd (c) Albert, 2025-
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/*
dc.subject.classificationFormació de les galàxiescat
dc.subject.classificationRefredamentcat
dc.subject.classificationTreballs de fi de graucat
dc.subject.otherGalaxy formationeng
dc.subject.otherCoolingeng
dc.subject.otherBachelor's theseseng
dc.titleCosmological cooling of gas within dark matter haloseng
dc.typeinfo:eu-repo/semantics/bachelorThesisca
dc.rights.accessRightsinfo:eu-repo/semantics/openAccessca
Appears in Collections:Treballs Finals de Grau (TFG) - Física

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