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[{"key": "dc.contributor.advisor", "value": "Kainulainen, Kimmo", "language": "", "element": "contributor", "qualifier": "advisor", "schema": "dc"}, {"key": "dc.contributor.author", "value": "Tenhu, Linda", "language": "", "element": "contributor", "qualifier": "author", "schema": "dc"}, {"key": "dc.date.accessioned", "value": "2018-10-24T06:55:58Z", "language": null, "element": "date", "qualifier": "accessioned", "schema": "dc"}, {"key": "dc.date.available", "value": "2018-10-24T06:55:58Z", "language": null, "element": "date", "qualifier": "available", "schema": "dc"}, {"key": "dc.date.issued", "value": "2018", "language": "", "element": "date", "qualifier": "issued", "schema": "dc"}, {"key": "dc.identifier.uri", "value": "https://jyx.jyu.fi/handle/123456789/59920", "language": null, "element": "identifier", "qualifier": "uri", "schema": "dc"}, {"key": "dc.description.abstract", "value": "T\u00e4ll\u00e4 hetkell\u00e4 universumin laajenemisnopeudessa eli Hubblen parametrin arvossa on havaittu noin 3,6 standardipoikkeaman ero paikallisen (et\u00e4isyystikapuut) sek\u00e4 globaalin (kosminen taustas\u00e4teily) mittaustavan v\u00e4lill\u00e4. T\u00e4ss\u00e4 pro gradu -tutkielmassa esitet\u00e4\u00e4n kosmologisesta standardimallista poiketen ep\u00e4homogeeninen wLTB-malli, jonka avulla kyseist\u00e4 eroa voidaan selitt\u00e4\u00e4. wLTB-mallissa pystyt\u00e4\u00e4n ratkaisemaan Einsteinin kentt\u00e4yht\u00e4l\u00f6t eksaktisti ep\u00e4homogeenisessa pallosymmetrisess\u00e4 tapauksessa, mik\u00e4 mahdollistaa paikasta riippuvan Hubblen parametrin arvon m\u00e4\u00e4ritt\u00e4misen ep\u00e4homogeenisen alueen, eli LTB-kuplan sis\u00e4ll\u00e4. Osoittautuu, ett\u00e4 ymp\u00e4rist\u00f6\u00e4\u00e4n harvempi kupla kasvattaa paikallista Hubblen vakion arvoa ja voi siten selitt\u00e4\u00e4 eroa havaintojen v\u00e4lill\u00e4. Mielivaltainen ep\u00e4homogenia eik\u00e4 mielivaltainen havainnoijan sijainti ep\u00e4homogenian sis\u00e4ll\u00e4 ole kuitenkaan sallittu. Tulevaisuuden haasteena on sovittaa homogeniaan kohdistuvat rajoitukset yhteen havaitun Hubblen vakion poik- keaman kanssa.", "language": "fi", "element": "description", "qualifier": "abstract", "schema": "dc"}, {"key": "dc.description.abstract", "value": "A tension of 3.6 standard deviation has been observed between the local (distance ladder) and global (cosmic microwave background) measurements in the expansion rate of the universe i.e. the present-day Hubble parameter value H0. In this Master\u2019s Thesis, depart from the Standard Model of Cosmology, an inhomogeneous cosmological wLTB model is introduced to explain the observed tension. The wLTB model enables one to solve the Einstein\u2019s field equations exactly in an inhomogeneous but spherically symmetric case. This makes it possible to determine the current Hubble parameter value inside an inhomogeneous area called LTB bubble. It turns out that an underdense bubble increases the local Hubble parameter value and thus makes the wLTB model a possible candidate that can explain the Hubble parameter tension. However, arbitrary inhomogeneities as well as observer\u2019s arbitrary locations inside the bubble are not allowed. In the future, the challenge is to fit the restrictions for the inhomogeneity and the Hubble parameter observational data together.", "language": "en", "element": "description", "qualifier": "abstract", "schema": "dc"}, {"key": "dc.description.provenance", "value": "Submitted by Paivi Vuorio (paelvuor@jyu.fi) on 2018-10-24T06:55:58Z\nNo. of bitstreams: 0", "language": "en", "element": "description", "qualifier": "provenance", "schema": "dc"}, {"key": "dc.description.provenance", "value": "Made available in DSpace on 2018-10-24T06:55:58Z (GMT). No. of bitstreams: 0\n Previous issue date: 2018", "language": "en", "element": "description", "qualifier": "provenance", "schema": "dc"}, {"key": "dc.format.extent", "value": "107", "language": "", "element": "format", "qualifier": "extent", "schema": "dc"}, {"key": "dc.format.mimetype", "value": "application/pdf", "language": null, "element": "format", "qualifier": "mimetype", "schema": "dc"}, {"key": "dc.language.iso", "value": "eng", "language": null, "element": "language", "qualifier": "iso", "schema": "dc"}, {"key": "dc.rights", "value": "In Copyright", "language": "en", "element": "rights", "qualifier": null, "schema": "dc"}, {"key": "dc.subject.other", "value": "inhomogeneous cosmological models", "language": "", "element": "subject", "qualifier": "other", "schema": "dc"}, {"key": "dc.subject.other", "value": "Hubble parameter", "language": "", "element": "subject", "qualifier": "other", "schema": "dc"}, {"key": "dc.title", "value": "On explaining the tension in the observations of the Hubble parameter by the wLTB model", "language": "", "element": "title", "qualifier": null, "schema": "dc"}, {"key": "dc.type", "value": "master thesis", "language": null, "element": "type", "qualifier": null, "schema": "dc"}, {"key": "dc.identifier.urn", "value": "URN:NBN:fi:jyu-201810244509", "language": "", "element": "identifier", "qualifier": "urn", "schema": "dc"}, {"key": "dc.type.ontasot", "value": "Pro gradu -tutkielma", "language": "fi", "element": "type", "qualifier": "ontasot", "schema": "dc"}, {"key": "dc.type.ontasot", "value": "Master\u2019s thesis", "language": "en", "element": "type", "qualifier": "ontasot", "schema": "dc"}, {"key": "dc.contributor.faculty", "value": "Matemaattis-luonnontieteellinen tiedekunta", "language": "fi", "element": "contributor", "qualifier": "faculty", "schema": "dc"}, {"key": "dc.contributor.faculty", "value": "Faculty of Sciences", "language": "en", "element": "contributor", "qualifier": "faculty", "schema": "dc"}, {"key": "dc.contributor.department", "value": "Fysiikan laitos", "language": "fi", "element": "contributor", "qualifier": "department", "schema": "dc"}, {"key": "dc.contributor.department", "value": "Department of Physics", "language": "en", "element": "contributor", "qualifier": "department", "schema": "dc"}, {"key": "dc.contributor.organization", "value": "Jyv\u00e4skyl\u00e4n yliopisto", "language": "fi", "element": "contributor", "qualifier": "organization", "schema": "dc"}, {"key": "dc.contributor.organization", "value": "University of Jyv\u00e4skyl\u00e4", "language": "en", "element": "contributor", "qualifier": "organization", "schema": "dc"}, {"key": "dc.subject.discipline", "value": "Teoreettinen fysiikka", "language": "fi", "element": "subject", "qualifier": "discipline", "schema": "dc"}, {"key": "dc.subject.discipline", "value": "Theoretical Physics", "language": "en", "element": "subject", "qualifier": "discipline", "schema": "dc"}, {"key": "yvv.contractresearch.funding", "value": "0", "language": "", "element": "contractresearch", "qualifier": "funding", "schema": "yvv"}, {"key": "dc.type.coar", "value": "http://purl.org/coar/resource_type/c_bdcc", "language": null, "element": "type", "qualifier": "coar", "schema": "dc"}, {"key": "dc.rights.accesslevel", "value": "openAccess", "language": null, "element": "rights", "qualifier": "accesslevel", "schema": "dc"}, {"key": "dc.type.publication", "value": "masterThesis", "language": null, "element": "type", "qualifier": "publication", "schema": "dc"}, {"key": "dc.subject.oppiainekoodi", "value": "4024", "language": "", "element": "subject", "qualifier": "oppiainekoodi", "schema": "dc"}, {"key": "dc.subject.yso", "value": "kosmologia", "language": null, "element": "subject", "qualifier": "yso", "schema": "dc"}, {"key": "dc.subject.yso", "value": "cosmology", "language": null, "element": "subject", "qualifier": "yso", "schema": "dc"}, {"key": "dc.format.content", "value": "fulltext", "language": null, "element": "format", "qualifier": "content", "schema": "dc"}, {"key": "dc.rights.url", "value": "https://rightsstatements.org/page/InC/1.0/", "language": null, "element": "rights", "qualifier": "url", "schema": "dc"}, {"key": "dc.type.okm", "value": "G2", "language": null, "element": "type", "qualifier": "okm", "schema": "dc"}]
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