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Full Mueller imaging: direction dependent corrections in polarimetric radio imaging
Magnetic fields pervade the universe, spanning a multitude of scales from the dipolar field on Earth, to the largest gravitationally bound structures such as galaxy clusters [1]. The magnetic fields play a vital role in the evolution of these astronomical systems. In addition to the multitude of sca...
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| Format: | Thesis |
| Language: | English |
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Department of Astronomy
2018
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| _version_ | 1867614421301329920 |
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| access_status_str | Open Access |
| author | Jagannathan, Preshanth |
| author2 | Taylor, Andrew Russell |
| author_browse | Jagannathan, Preshanth Taylor, Andrew Russell |
| author_facet | Taylor, Andrew Russell Jagannathan, Preshanth |
| author_sort | Jagannathan, Preshanth |
| collection | Thesis |
| description | Magnetic fields pervade the universe, spanning a multitude of scales from the dipolar field on Earth, to the largest gravitationally bound structures such as galaxy clusters [1]. The magnetic fields play a vital role in the evolution of these astronomical systems. In addition to the multitude of scales, magnetic fields are present in different astronomical systems of varying strengths. The strongest observed astronomical magnetic fields are in neutron stars with a field strength of ≈ 1015 G [2], far higher than any man-made fields till date. In stark contrast magnetic fields in the interstellar medium while ubiquitous are only a few µG in field strength. Many fundamental processes in astrophysics have magnetism at their heart, be it cosmic ray particle acceleration, star formation, or the launch of radio galaxy jets, pulsars, etc. One key fundamental process that allows us to detect and characterize cosmic magnetic fields with radio astronomy is the polarization of synchrotron radiation. Synchrotron radiation is intrinsically polarized broadband continuum radiation emitted by relativistic charged particles accelerated by the presence of magnetic fields. The emissivity of the synchrotron radiation is tied to the magnetic field strength B and the spectral index α (defined such that the flux density S ∝ ν −α ) such that ε ∝ B 1+α . |
| format | Thesis |
| id | oai:open.uct.ac.za:11427/28421 |
| institution | University of Cape Town (South Africa) |
| language | eng |
| last_indexed | 2026-06-10T12:51:46.545Z |
| license_str | Not specified — see source repository |
| provenance_str_mv | Harvested via OAI-PMH from UCTD — University of Cape Town Open Access Repository |
| publishDate | 2018 |
| publishDateRange | 2018 |
| publishDateSort | 2018 |
| 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:11427/28421 Full Mueller imaging: direction dependent corrections in polarimetric radio imaging Jagannathan, Preshanth Taylor, Andrew Russell Polarimetric Radio Imaging astronomy Magnetic fields pervade the universe, spanning a multitude of scales from the dipolar field on Earth, to the largest gravitationally bound structures such as galaxy clusters [1]. The magnetic fields play a vital role in the evolution of these astronomical systems. In addition to the multitude of scales, magnetic fields are present in different astronomical systems of varying strengths. The strongest observed astronomical magnetic fields are in neutron stars with a field strength of ≈ 1015 G [2], far higher than any man-made fields till date. In stark contrast magnetic fields in the interstellar medium while ubiquitous are only a few µG in field strength. Many fundamental processes in astrophysics have magnetism at their heart, be it cosmic ray particle acceleration, star formation, or the launch of radio galaxy jets, pulsars, etc. One key fundamental process that allows us to detect and characterize cosmic magnetic fields with radio astronomy is the polarization of synchrotron radiation. Synchrotron radiation is intrinsically polarized broadband continuum radiation emitted by relativistic charged particles accelerated by the presence of magnetic fields. The emissivity of the synchrotron radiation is tied to the magnetic field strength B and the spectral index α (defined such that the flux density S ∝ ν −α ) such that ε ∝ B 1+α . 2018-09-06T13:26:31Z 2018-09-06T13:26:31Z 2018 2018-08-24T10:05:27Z Doctoral Thesis Doctoral PhD http://hdl.handle.net/11427/28421 eng application/pdf Department of Astronomy Faculty of Science University of Cape Town |
| spellingShingle | Polarimetric Radio Imaging astronomy Jagannathan, Preshanth Full Mueller imaging: direction dependent corrections in polarimetric radio imaging |
| thesis_degree_str | Doctoral |
| title | Full Mueller imaging: direction dependent corrections in polarimetric radio imaging |
| title_full | Full Mueller imaging: direction dependent corrections in polarimetric radio imaging |
| title_fullStr | Full Mueller imaging: direction dependent corrections in polarimetric radio imaging |
| title_full_unstemmed | Full Mueller imaging: direction dependent corrections in polarimetric radio imaging |
| title_short | Full Mueller imaging: direction dependent corrections in polarimetric radio imaging |
| title_sort | full mueller imaging direction dependent corrections in polarimetric radio imaging |
| topic | Polarimetric Radio Imaging astronomy |
| url | http://hdl.handle.net/11427/28421 |
| work_keys_str_mv | AT jagannathanpreshanth fullmuellerimagingdirectiondependentcorrectionsinpolarimetricradioimaging |