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[{"key": "dc.contributor.author", "value": "Heikkil\u00e4, Elena", "language": null, "element": "contributor", "qualifier": "author", "schema": "dc"}, {"key": "dc.date.accessioned", "value": "2009-11-11T12:53:19Z", "language": null, "element": "date", "qualifier": "accessioned", "schema": "dc"}, {"key": "dc.date.available", "value": "2009-11-11T12:53:19Z", "language": null, "element": "date", "qualifier": "available", "schema": "dc"}, {"key": "dc.date.issued", "value": "2009", "language": null, "element": "date", "qualifier": "issued", "schema": "dc"}, {"key": "dc.identifier.uri", "value": "https://jyx.jyu.fi/handle/123456789/22372", "language": null, "element": "identifier", "qualifier": "uri", "schema": "dc"}, {"key": "dc.description.abstract", "value": "This thesis is about deriving a few equations of state for white\r\ndwarfs below the regime of neutron drip. White dwarfs - also called\r\ndegenerate dwarfs, composed mostly of electron-degenerate matter - \r\nare luminous and the color of the light they are emitting is white,\r\nhence their name. Because of the relatively enormous density, the\r\ngravitational potential of a white dwarf causes a collapse.\r\nWhite dwarfs are classified as compact objects, meaning that their\r\nlife begins when a star dies, and are therefore considered as\r\none possibility of a final stage of stellar evolution since they\r\nare considered static over the lifetime of the Universe. Star death is\r\na point where the most of its nuclear fuel has been consumed. After\r\nthe birth, white dwarfs are slowly cooling, radiating away their\r\nresidual thermal energy.\r\nWhite dwarfs resist the gravitational collapse with electron\r\ndegeneracy pressure. The temperature of white dwarfs is much\r\nhigher than that of normal stars. These properties, together with\r\nexceedingly small size, are characteristic of white dwarfs. Cooling of\r\nwhite dwarfs offers information of solid state physics in a new setting\r\n- the circumstances of an original star can not be built up\r\nin a laboratory. Also, it would not be possible to realize the\r\ndistance, which includes many advantages in sketching timescales\r\nand fundamental interactions by observation. More over, the\r\nevolution and the equation of state of white dwarfs provide us with\r\nmore understanding of matter and physics describing the Universe.\r\nIn this study, the equation of state for white dwarf matter\r\nis derived first by treating the matter as ideal Fermi gas, then\r\nincluding also electrostatic forces and considering the effects of\r\ninverse \u03b2-decay. We conclude with an overview of the equation\r\nof gravitational potential energy arising from hydrostatic equilibrium.\r\nThe accuracy of the equation of state was concluded to depend on\r\nwhich interactions and phenomenon are included in the consideration.\r\nOn the other hand, choosing the white dwarf model for\r\nan application depends significantly on the density of the matter,\r\nas well. The equations of state of ideal Fermi gas, with Coulomb\r\ncorrection and with the inverse \u03b2-decay correction were concluded to\r\nbe accurate enough to provide a quantitatively adequate description\r\nof the phenomenon.\u00a0\u00a0", "language": "en", "element": "description", "qualifier": "abstract", "schema": "dc"}, {"key": "dc.description.provenance", "value": "Submitted by Veli-Matti Hakkinen (veanha@cc.jyu.fi) on 2009-11-11T12:53:19Z\r\nNo. of bitstreams: 2\r\nURN_NBN_fi_jyu-200911024335.pdf: 355547 bytes, checksum: 52c0c182c22512288c16bb59288e8b2f (MD5)\r\nlicense.xml: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5)", "language": "en", "element": "description", "qualifier": "provenance", "schema": "dc"}, {"key": "dc.description.provenance", "value": "Made available in DSpace on 2009-11-11T12:53:19Z (GMT). No. of bitstreams: 2\r\nURN_NBN_fi_jyu-200911024335.pdf: 355547 bytes, checksum: 52c0c182c22512288c16bb59288e8b2f (MD5)\r\nlicense.xml: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5)", "language": "en", "element": "description", "qualifier": "provenance", "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": "Condensed matter physics", "language": "en", "element": "subject", "qualifier": "other", "schema": "dc"}, {"key": "dc.subject.other", "value": "Astrophysics", "language": "en", "element": "subject", "qualifier": "other", "schema": "dc"}, {"key": "dc.title", "value": "Equations of State for White Dwarfs", "language": null, "element": "title", "qualifier": null, "schema": "dc"}, {"key": "dc.type", "value": "bachelor thesis", "language": null, "element": "type", "qualifier": null, "schema": "dc"}, {"key": "dc.identifier.urn", "value": "URN:NBN:fi:jyu-200911024335", "language": null, "element": "identifier", "qualifier": "urn", "schema": "dc"}, {"key": "dc.type.dcmitype", "value": "Text", "language": "en", "element": "type", "qualifier": "dcmitype", "schema": "dc"}, {"key": "dc.type.ontasot", "value": "Bachelor's thesis", "language": "en", "element": "type", "qualifier": "ontasot", "schema": "dc"}, {"key": "dc.type.ontasot", "value": "Kandidaatintutkielma", "language": "fi", "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 Mathematics and Science", "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.organization", "value": "University of Jyv\u00e4skyl\u00e4", "language": "en", "element": "contributor", "qualifier": "organization", "schema": "dc"}, {"key": "dc.contributor.organization", "value": "Jyv\u00e4skyl\u00e4n yliopisto", "language": "fi", "element": "contributor", "qualifier": "organization", "schema": "dc"}, {"key": "dc.subject.discipline", "value": "Fysiikka", "language": "fi", "element": "subject", "qualifier": "discipline", "schema": "dc"}, {"key": "dc.type.coar", "value": "http://purl.org/coar/resource_type/c_7a1f", "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": "bachelorThesis", "language": null, "element": "type", "qualifier": "publication", "schema": "dc"}, {"key": "dc.rights.url", "value": "https://rightsstatements.org/page/InC/1.0/", "language": null, "element": "rights", "qualifier": "url", "schema": "dc"}]
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