Investigation of the Mode-Switching Phenomenon in Pulsar B0329+54 Through Polarimetric Analysis. (arXiv:1901.08677v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Brinkman_C/0/1/0/all/0/1">Casey Brinkman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mitra_D/0/1/0/all/0/1">Dipanjan Mitra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rankin_J/0/1/0/all/0/1">Joanna Rankin</a>
The phenomenon of profile mode switching in pulsars, where the stable average
pulse profile changes to another stable state on the timescale of a pulsar’s
period, remains poorly understood. We sought to understand how pulsars undergo
profile mode switching through a comparative analysis of the polarization and
geometry of the two different profile modes of PSR B0329+54. The polarization
behavior and fitted parameters of the rotation-vector model remain constant
between modes, and the emission height remains constant as well. These
similarities lend support to a model of pair production in the surface plasma
that would cause a change in the available electrons and therefore the
differential emission intensity.
The phenomenon of profile mode switching in pulsars, where the stable average
pulse profile changes to another stable state on the timescale of a pulsar’s
period, remains poorly understood. We sought to understand how pulsars undergo
profile mode switching through a comparative analysis of the polarization and
geometry of the two different profile modes of PSR B0329+54. The polarization
behavior and fitted parameters of the rotation-vector model remain constant
between modes, and the emission height remains constant as well. These
similarities lend support to a model of pair production in the surface plasma
that would cause a change in the available electrons and therefore the
differential emission intensity.
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