Full Mueller imaging: direction dependent corrections in polarimetric radio imaging

 

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dc.contributor.advisor Taylor, Andrew Russell
dc.contributor.author Jagannathan, Preshanth
dc.date.accessioned 2018-09-06T13:26:31Z
dc.date.available 2018-09-06T13:26:31Z
dc.date.issued 2018
dc.identifier.citation Jagannathan, P. 2018. Full Mueller imaging: direction dependent corrections in polarimetric radio imaging. University of Cape Town. en_ZA
dc.identifier.uri http://hdl.handle.net/11427/28421
dc.description.abstract 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 .
dc.language.iso eng
dc.subject.other Polarimetric Radio Imaging
dc.subject.other astronomy
dc.title Full Mueller imaging: direction dependent corrections in polarimetric radio imaging
dc.type Doctoral Thesis
dc.date.updated 2018-08-24T10:05:27Z
dc.publisher.institution University of Cape Town
dc.publisher.faculty Faculty of Science en_ZA
dc.publisher.department Department of Astronomy en_ZA
dc.type.qualificationlevel Doctoral
dc.type.qualificationname PhD
uct.type.filetype Text
uct.type.filetype Image
dc.identifier.apacitation Jagannathan, P. (2018). <i>Full Mueller imaging: direction dependent corrections in polarimetric radio imaging</i>. (). University of Cape Town ,Faculty of Science ,Department of Astronomy. Retrieved from http://hdl.handle.net/11427/28421 en_ZA
dc.identifier.chicagocitation Jagannathan, Preshanth. <i>"Full Mueller imaging: direction dependent corrections in polarimetric radio imaging."</i> ., University of Cape Town ,Faculty of Science ,Department of Astronomy, 2018. http://hdl.handle.net/11427/28421 en_ZA
dc.identifier.vancouvercitation Jagannathan P. Full Mueller imaging: direction dependent corrections in polarimetric radio imaging. []. University of Cape Town ,Faculty of Science ,Department of Astronomy, 2018 [cited yyyy month dd]. Available from: http://hdl.handle.net/11427/28421 en_ZA
dc.identifier.ris TY - Thesis / Dissertation AU - Jagannathan, Preshanth AB - 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 . DA - 2018 DB - OpenUCT DP - University of Cape Town LK - https://open.uct.ac.za PB - University of Cape Town PY - 2018 T1 - Full Mueller imaging: direction dependent corrections in polarimetric radio imaging TI - Full Mueller imaging: direction dependent corrections in polarimetric radio imaging UR - http://hdl.handle.net/11427/28421 ER - en_ZA


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