dc.contributor.advisor | Venter, C. | en_US |
dc.contributor.advisor | Harding, A.K. | en_US |
dc.contributor.advisor | Wadiasingh, Z. | en_US |
dc.contributor.author | Du Plessis, L. | en_US |
dc.date.accessioned | 2021-02-18T06:23:49Z | |
dc.date.available | 2021-02-18T06:23:49Z | |
dc.date.issued | 2020 | en_US |
dc.identifier.uri | https://orcid.org/0000-0002-5158-4152 | en_US |
dc.identifier.uri | http://hdl.handle.net/10394/36681 | |
dc.description | MSc (Astrophysical Sciences), North-West University, Potchefstroom Campus | |
dc.description.abstract | Marsh et al. (2016) detected radio and optical pulsations from the binary system AR Scorpii (AR Sco). This system, with an orbital period of 3.55 h, is composed of a cool, low-mass M-dwarf and a white dwarf with a spin period of 1.95 min. Buckley et al. (2017) found that the emission from the white dwarf is strongly linearly polarised (up to 40%) with periodically changing intensities. This periodic non-thermal emission is thought to be synchrotron emission (Buckley et al., 2017; Takata et al., 2017) that is powered by the highly magnetised \begin{equation} <> alpha=\left(86.6_{-2.8}^{+3.0}\right)^{\circ}
\end{equation} </>Using these observations, I was able to do rst-order spectral calculations to constrain
some of the parameters for the system. Lastly, using phase-resolved optical observations, I was
able to obtain and at the di erent orbital phases. | |
dc.language.iso | en | en_US |
dc.publisher | North-West University (South Africa) | en_US |
dc.title | Constraining the emission geometry and mass of the white Dwarf Pulsar AR Sco | en_US |
dc.type | Thesis | en_US |
dc.description.thesistype | Masters | en_US |
dc.contributor.researchID | 26594080 - Wadiasingh, Zorawar (Supervisor) | en_US |