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Cosmic microwave background anisotropies in the presence of a weak magnetic field
Bibliography: leaves 87-90.
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| Format: | Thesis |
| Language: | English |
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Department of Mathematics and Applied Mathematics
2014
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| _version_ | 1867614453313306624 |
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| access_status_str | Open Access |
| author | Kahle, A |
| author_browse | Kahle, A |
| author_facet | Kahle, A |
| author_sort | Kahle, A |
| collection | Thesis |
| description | Bibliography: leaves 87-90. |
| format | Thesis |
| id | oai:open.uct.ac.za:11427/4894 |
| institution | University of Cape Town (South Africa) |
| language | eng |
| last_indexed | 2026-06-10T12:52:17.074Z |
| license_str | Not specified — see source repository |
| provenance_str_mv | Harvested via OAI-PMH from UCTD — University of Cape Town Open Access Repository |
| publishDate | 2014 |
| publishDateRange | 2014 |
| publishDateSort | 2014 |
| publisher | Department of Mathematics and Applied Mathematics |
| publisherStr | Department of Mathematics and Applied Mathematics |
| record_format | dspace |
| source_str | UCTD — University of Cape Town Open Access Repository |
| spelling | oai:open.uct.ac.za:11427/4894 Cosmic microwave background anisotropies in the presence of a weak magnetic field Kahle, A Mathematics and Applied Mathematics Bibliography: leaves 87-90. One of the questions cosmology still has not satisfactorily resolved is the origin of magnetic fields in the universe. These have been observed at all scales where man has c:evised means to observe them, from stellar scales, to intergalactic and intercluster scales. Indeed, there is no reason to believe that they are not present, at some level, at even larger scales. However, a satisfactory explanation for their origin is yet to be found. The two most popular theories for the creation of these magnetic fields, namely the Galactic dynamo, and primordial field amplification, both rely on the presence of a seed field, which they then amplify. However, the galactic dynamo requires a far weaker seed field compared to primordial field amplification. It would thus be helpful, in trying to understand magnetogenesis, if one could discover some means to detect such a seed field. One way to do so would be to search for a signature that such a magnetic field might leave on the CMB, and then look for the presence of this signature in CMB observations. This is the principal aim of this thesis. 2014-07-31T08:08:09Z 2014-07-31T08:08:09Z 2003 Master Thesis Masters MSc http://hdl.handle.net/11427/4894 eng application/pdf Department of Mathematics and Applied Mathematics Faculty of Science University of Cape Town |
| spellingShingle | Mathematics and Applied Mathematics Kahle, A Cosmic microwave background anisotropies in the presence of a weak magnetic field |
| thesis_degree_str | Master's |
| title | Cosmic microwave background anisotropies in the presence of a weak magnetic field |
| title_full | Cosmic microwave background anisotropies in the presence of a weak magnetic field |
| title_fullStr | Cosmic microwave background anisotropies in the presence of a weak magnetic field |
| title_full_unstemmed | Cosmic microwave background anisotropies in the presence of a weak magnetic field |
| title_short | Cosmic microwave background anisotropies in the presence of a weak magnetic field |
| title_sort | cosmic microwave background anisotropies in the presence of a weak magnetic field |
| topic | Mathematics and Applied Mathematics |
| url | http://hdl.handle.net/11427/4894 |
| work_keys_str_mv | AT kahlea cosmicmicrowavebackgroundanisotropiesinthepresenceofaweakmagneticfield |