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Constraining the emission geometry and mass of the white Dwarf Pulsar AR Sco

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North-West University (South Africa)

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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.

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MSc (Astrophysical Sciences), North-West University, Potchefstroom Campus

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