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On the model for U Geminorum
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,...
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| Format: | Thesis |
| Language: | English |
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Department of Astronomy
2016
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| _version_ | 1867613324695306240 |
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| access_status_str | Open Access |
| author | Harwood, John Malcolm |
| author2 | Warner, Brian |
| author_browse | Harwood, John Malcolm Warner, Brian |
| author_facet | Warner, Brian Harwood, John Malcolm |
| author_sort | Harwood, John Malcolm |
| collection | Thesis |
| description | 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. |
| format | Thesis |
| id | oai:open.uct.ac.za:11427/18324 |
| institution | University of Cape Town (South Africa) |
| language | eng |
| last_indexed | 2026-06-10T12:34:20.437Z |
| license_str | Not specified — see source repository |
| provenance_str_mv | Harvested via OAI-PMH from UCTD — University of Cape Town Open Access Repository |
| publishDate | 2016 |
| publishDateRange | 2016 |
| publishDateSort | 2016 |
| publisher | Department of Astronomy |
| publisherStr | Department of Astronomy |
| record_format | dspace |
| source_str | UCTD — University of Cape Town Open Access Repository |
| spelling | oai:open.uct.ac.za:11427/18324 On the model for U Geminorum Harwood, John Malcolm Warner, Brian Astronomy 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. 2016-03-28T14:42:52Z 2016-03-28T14:42:52Z 1973 Master Thesis Masters MSc http://hdl.handle.net/11427/18324 eng application/pdf Department of Astronomy Faculty of Science University of Cape Town |
| spellingShingle | Astronomy Harwood, John Malcolm On the model for U Geminorum |
| thesis_degree_str | Master's |
| title | On the model for U Geminorum |
| title_full | On the model for U Geminorum |
| title_fullStr | On the model for U Geminorum |
| title_full_unstemmed | On the model for U Geminorum |
| title_short | On the model for U Geminorum |
| title_sort | on the model for u geminorum |
| topic | Astronomy |
| url | http://hdl.handle.net/11427/18324 |
| work_keys_str_mv | AT harwoodjohnmalcolm onthemodelforugeminorum |