Non-radial Oscillations in Radio Pulsars

Details Non-radial Oscillations in Radio Pulsars Non-radial Oscillations in Radio Pulsars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21545316r&link_type=abstract

American Astronomical Society, AAS Meeting #215, #453.16; Bulletin of the American Astronomical Society, Vol. 42, p.465

Astronomy and Astrophysics

Astronomy

Scientific paper

We propose a model for radio pulsars in which non-radial oscillations of high spherical degree (l) are aligned to the magnetic axis of a spinning neutron star. The model of non-radial oscillations is able to reproduce the fixed and variable subpulse structure like those observed in single pulse observations of pulsars. Observations show that many pulsars emit radio waves that appear to be the superposition of two linearly polarized emission modes with orthogonal polarization angles. We propose that pulsational displacements of stellar material modulate the pulsar emission, and we apply this modulation to a linearly-polarized mode of emission, such as curvature radiation. We introduce a second polarization mode, orthogonal to the first, that is modulated by pulsational velocities. These modes can be combined in superposition to model the observed Stokes parameters.
Using our model, we analyzed and fit single pulse measurements of several pulsars, including PSR B0943+10 and PSR B1702-19. Analysis shows undocumented behavior in both stars. In the case of PSR B0943+10, we observe a splitting of the subpulse frequency and a splitting in the driftband; PSR B1702-19 shows several subpulse frequencies. We used a least squares fitting algorithm to fit the parameters in our model to amplitude-normalized single pulse data on both these pulsars. We found that the parameters in our model fall into two categories: pulsational and geometrical, and that the two types of parameters are largely independent. We created synthetic data that reproduce the stable features of the observations, including the pulse shape, the polarization angles, and the orthogonal mode morphology.

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