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Studium atmosfér Be hvězd
dc.contributor.advisorKubát, Jiří
dc.creatorSokolovičová, Júlia
dc.date.accessioned2017-03-17T12:06:07Z
dc.date.available2017-03-17T12:06:07Z
dc.date.issued2006
dc.identifier.urihttp://hdl.handle.net/20.500.11956/3396
dc.description.abstractBe stars are a group of hot, massive, emission-line stars characterized by intense radiatively-driven stellar wind and extremely rapid rotation. The typical emission in the Balmer series arises in a thin equatorial disc around the star. The detailed structure and most of all origin of the disc are still unknown. The aim of this thesis is to give a thorough review of the main directions of research into the eld. We describe observational features that set Be stars apart from the rest of the B spectral class: Balmer emission, linear polarization, infrared excess and superionized resonance lines in the far UV range; also main physical characteristics of the underlying star, and variability. We discuss the so-called Be phenomenon - the unknown mechanism creating the emission-producing circumstellar disc in Be stars, and providine an overview of the most successful models attempting to explain the Be phenomenon. Finally we discuss the rotation law of the disc and its importance in placing a physical constraint on possible models for Be stars, and apply one of the examined rotation parameter nding methods.en_US
dc.languageEnglishcs_CZ
dc.language.isoen_US
dc.publisherUniverzita Karlova, Matematicko-fyzikální fakultacs_CZ
dc.titleStudium atmosfér Be hvězden_US
dc.typediplomová prácecs_CZ
dcterms.created2006
dcterms.dateAccepted2006-02-15
dc.description.departmentAstronomical Institute of Charles Universityen_US
dc.description.departmentAstronomický ústav UKcs_CZ
dc.description.facultyFaculty of Mathematics and Physicsen_US
dc.description.facultyMatematicko-fyzikální fakultacs_CZ
dc.identifier.repId41615
dc.title.translatedStudium atmosfér Be hvězdcs_CZ
dc.contributor.refereeMayer, Pavel
dc.identifier.aleph001138805
thesis.degree.nameMgr.
thesis.degree.levelmagisterskécs_CZ
thesis.degree.disciplineAstronomy and astrophysicsen_US
thesis.degree.disciplineAstronomie a astrofyzikacs_CZ
thesis.degree.programPhysicsen_US
thesis.degree.programFyzikacs_CZ
uk.thesis.typediplomová prácecs_CZ
uk.taxonomy.organization-csMatematicko-fyzikální fakulta::Astronomický ústav UKcs_CZ
uk.taxonomy.organization-enFaculty of Mathematics and Physics::Astronomical Institute of Charles Universityen_US
uk.faculty-name.csMatematicko-fyzikální fakultacs_CZ
uk.faculty-name.enFaculty of Mathematics and Physicsen_US
uk.faculty-abbr.csMFFcs_CZ
uk.degree-discipline.csAstronomie a astrofyzikacs_CZ
uk.degree-discipline.enAstronomy and astrophysicsen_US
uk.degree-program.csFyzikacs_CZ
uk.degree-program.enPhysicsen_US
thesis.grade.csVelmi dobřecs_CZ
thesis.grade.enVery gooden_US
uk.abstract.enBe stars are a group of hot, massive, emission-line stars characterized by intense radiatively-driven stellar wind and extremely rapid rotation. The typical emission in the Balmer series arises in a thin equatorial disc around the star. The detailed structure and most of all origin of the disc are still unknown. The aim of this thesis is to give a thorough review of the main directions of research into the eld. We describe observational features that set Be stars apart from the rest of the B spectral class: Balmer emission, linear polarization, infrared excess and superionized resonance lines in the far UV range; also main physical characteristics of the underlying star, and variability. We discuss the so-called Be phenomenon - the unknown mechanism creating the emission-producing circumstellar disc in Be stars, and providine an overview of the most successful models attempting to explain the Be phenomenon. Finally we discuss the rotation law of the disc and its importance in placing a physical constraint on possible models for Be stars, and apply one of the examined rotation parameter nding methods.en_US
uk.publication.placePrahacs_CZ
uk.grantorUniverzita Karlova, Matematicko-fyzikální fakulta, Astronomický ústav UKcs_CZ
dc.identifier.lisID990011388050106986


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