Can the Tremaine - Weinberg method be used to determine the pattern speed of the bar and the spiral arms of the Milky Way?

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dc.contributor.advisorFigueras Siñol, Francesca
dc.contributor.advisorAntoja Castelltort, M. Teresa
dc.contributor.advisorRomero Gómez, Mercè
dc.contributor.advisorRoca Fàbrega, Santi
dc.contributor.authorReina Campos, Marta
dc.date.accessioned2020-01-07T16:06:39Z
dc.date.available2020-01-07T16:06:39Z
dc.date.issued2016-06
dc.descriptionMàster Oficial d'Astrofísica, Física de Partícules i Cosmologia, Facultat de Física, Universitat de Barcelona, Curs: 2015-2016, Tutors: Francesca Figueras, Teresa Antoja, Mercè Romero-Gómez, Santi Roca-Fàbregaca
dc.description.abstractThe pattern speed of the non-axisymmetric structures of the galactic disc is a key parameter to understand the dynamics in the MilkyWay. For neither the Galactic bar nor the spiral arms it is well determined. All previous determinations have large uncertainties associated avoiding to shed some light on the nature of these structures.ca
dc.format.extent17 p.
dc.format.mimetypeapplication/pdf
dc.identifier.urihttps://hdl.handle.net/2445/147137
dc.language.isoengca
dc.rightscc-by-nc-nd (c) Reina, 2016
dc.rights.accessRightsinfo:eu-repo/semantics/openAccessca
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/es/*
dc.sourceMàster Oficial - Astrofísica, Física de Partícules i Cosmologia
dc.subject.classificationGalàxiescat
dc.subject.classificationVia Làctiacat
dc.subject.classificationGalàxia espiralcat
dc.subject.classificationTreballs de fi de màstercat
dc.subject.classificationGalaxieseng
dc.subject.otherMilky Wayeng
dc.subject.otherSpiral galaxyeng
dc.subject.otherMaster's theseseng
dc.titleCan the Tremaine - Weinberg method be used to determine the pattern speed of the bar and the spiral arms of the Milky Way?eng
dc.typeinfo:eu-repo/semantics/masterThesisca

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