Statistics of the individual-pulse polarization based on propagation effects in pulsar magnetosphere

Details Statistics of the individual-pulse polarization based on propagation effects in pulsar magnetosphere Statistics of the individual-pulse polarization based on propagation effects in pulsar magnetosphere

2006-03-13

arxiv.org/abs/astro-ph/0603301v1

Mon.Not.Roy.Astron.Soc.368:1764-1772,2006

Astronomy and Astrophysics

Astrophysics

15 pages, 6 figures. Accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2006.10246.x

Pulsar radio emission is modelled as a sum of two completely polarized non-orthogonal modes with the randomly varying Stokes parameters and intensity ratio. The modes are the result of polarization evolution of the original natural waves in the hot magnetized weakly inhomogeneous plasma of pulsar magnetosphere. In the course of wave mode coupling, the linearly polarized natural waves acquire purely orthogonal elliptical polarizations. Further on, as the waves pass through the cyclotron resonance, they become non-orthogonal. The pulse-to-pulse fluctuations of the final polarization characteristics and the intensity ratio of the modes are attributed to the temporal fluctuations in the plasma flow. The model suggested allows to reproduce the basic features of the one-dimensional distributions of the individual-pulse polarization characteristics. Besides that, propagation origin of pulsar polarization implies a certain correlation between the mode ellipticity and position angle. On a qualitative level, for different sets of parameters, the expected correlations appear compatible with the observed ones. Further theoretical studies are necessary to establish the quantitative correspondence of the model to the observational results and to develop a technique of diagnostics of pulsar plasma on this basis.

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