On the model for U Geminorum

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dc.contributor.advisorWarner, Brianen_ZA
dc.contributor.authorHarwood, John Malcolmen_ZA
dc.date.accessioned2016-03-28T14:42:52Z
dc.date.available2016-03-28T14:42:52Z
dc.date.issued1973en_ZA
dc.description.abstractThe term cataclysmic variable comprises several types of variable star - novae, recurrent novae, dwarf novae; and to these we add the nova-like variables, stars which exhibit many of the characteristics of the novae but which have not been observed to erupt. U Geminorum, discovered by Hinds in 1855, is the nomotype of the dwarf novae. These stars are characterised by large, abrupt, temporary increases in brightness that occur erratically at intervals of ten days to a year or more. The dwarf novae are faint objects, few reaching 11th magnitude at maximum, whereas at minimum light most are fainter than 16th magnitude. Thus they are spectroscopically inaccessible to all but the largest telescopes. Conventional photometric techniques applied to these objects gave no information indicating their physical nature. The time-scale of the observations was so long that only the gross variations in brightness were detected. Much of the observing was undertaken by amateurs (Fig. 1), and from this work several of the basic features of this group have emerged.en_ZA
dc.identifier.apacitationHarwood, J. M. (1973). <i>On the model for U Geminorum</i>. (Thesis). University of Cape Town ,Faculty of Science ,Department of Astronomy. Retrieved from http://hdl.handle.net/11427/18324en_ZA
dc.identifier.chicagocitationHarwood, John Malcolm. <i>"On the model for U Geminorum."</i> Thesis., University of Cape Town ,Faculty of Science ,Department of Astronomy, 1973. http://hdl.handle.net/11427/18324en_ZA
dc.identifier.citationHarwood, J. 1973. On the model for U Geminorum. University of Cape Town.en_ZA
dc.identifier.ris TY - Thesis / Dissertation AU - Harwood, John Malcolm AB - The term cataclysmic variable comprises several types of variable star - novae, recurrent novae, dwarf novae; and to these we add the nova-like variables, stars which exhibit many of the characteristics of the novae but which have not been observed to erupt. U Geminorum, discovered by Hinds in 1855, is the nomotype of the dwarf novae. These stars are characterised by large, abrupt, temporary increases in brightness that occur erratically at intervals of ten days to a year or more. The dwarf novae are faint objects, few reaching 11th magnitude at maximum, whereas at minimum light most are fainter than 16th magnitude. Thus they are spectroscopically inaccessible to all but the largest telescopes. Conventional photometric techniques applied to these objects gave no information indicating their physical nature. The time-scale of the observations was so long that only the gross variations in brightness were detected. Much of the observing was undertaken by amateurs (Fig. 1), and from this work several of the basic features of this group have emerged. DA - 1973 DB - OpenUCT DP - University of Cape Town LK - https://open.uct.ac.za PB - University of Cape Town PY - 1973 T1 - On the model for U Geminorum TI - On the model for U Geminorum UR - http://hdl.handle.net/11427/18324 ER - en_ZA
dc.identifier.urihttp://hdl.handle.net/11427/18324
dc.identifier.vancouvercitationHarwood JM. On the model for U Geminorum. [Thesis]. University of Cape Town ,Faculty of Science ,Department of Astronomy, 1973 [cited yyyy month dd]. Available from: http://hdl.handle.net/11427/18324en_ZA
dc.language.isoengen_ZA
dc.publisher.departmentDepartment of Astronomyen_ZA
dc.publisher.facultyFaculty of Scienceen_ZA
dc.publisher.institutionUniversity of Cape Town
dc.subject.otherAstronomyen_ZA
dc.titleOn the model for U Geminorumen_ZA
dc.typeMaster Thesis
dc.type.qualificationlevelMasters
dc.type.qualificationnameMScen_ZA
uct.type.filetypeText
uct.type.filetypeImage
uct.type.publicationResearchen_ZA
uct.type.resourceThesisen_ZA
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