A NonRadial Oscillation Model for Radio Pulsars In

A Non-Radial Oscillation Model for Radio Pulsars In collaboration with Dr. J. Christopher Clemens University of North Carolina at Chapel Hill

Average Pulse Shapes

Polarization Properties Stinebring, D. R. , Cordes, J. M. , Rankin, J. M. , Weisberg, J. M. , & Boriakoff, V. 1984, Ap. JS, 55, 247

Drifting Subpulses

Vacuum Gap, Drifting Spark Model

Phase Shifts PSR 0320+39 Rapidly oscillating Ap star HR 3831 Edwards, R. T. , Stappers, B. W. , & van Leeuwen, A. G. J. 2003, A&A, 401, 321

Intensity and Velocity Variations The displacement (intensity) variations are described as: The velocity variations are described as: Where are spherical coordinates aligned to the magnetic axis of the star

Intensity Variations in WDs l = 1, m = 0 l = 2, m = 0

Polarization Geometry Displacements and velocities are aligned to magnetic pole Induced electric field (Eϕ) due to Eϕ = v x B(0) is orthogonal to Eθ Result: two orthogonal electric fields

Our Model

Single Pulse Behavior

PSR 0943+10: Data The: Single pulses Fourier Transform

PSR 0943+10: Dual Frequencies Two possibilities for a split subpulse frequency: 1. Two closely spaced independent frequencies 2. Combined frequency and amplitude or phase modulation of a single frequency

PSR B 0943+10 Pulsational and geometrical parameters are largely independent

Conclusions and Future Work Developed a physical model for pulsar morphology based on asteroseismological principles Conducted quantitative fitting of model to data Next step: fit more complex pulsar behavior, acquire data for definitive tests Subpulse phase correlation between both magnetic poles Subpulse frequency independent of observational radio frequency