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Session 50 - Pulsars in the UV and Visible.
Topical, Oral session, Wednesday, June 10

[50.02] The Vector Model of Pulsar Emission: Observations in i the UV and Visible

J. F. Dolan (LASP, NASA GSFC and Dept. Astron., SDSU)

Isolated pulsars radiate by accelerating particles away from the neutron star rather than by accreting material from a companion. According to the vector model of pulsar emission [F. G. Smith, 1986, MNRAS, 219, 729; 1991, Comm. Ap., 15, 207; A. Lyne amp; F. G. Smith, 1990, "Pulsar Astronomy", Cambridge U. Press], the IR to gamma-ray emission from isolated pulsars comes from a region near their velocity- of-light co-rotation cylinder. (The radio emission is generated in a different region over the magnetic poles.) A comparison of the predictions of the vector model with HST observations of the Crab pulsar and PSR B0540-69 in the UV and visible shows that the frequency dependence of both the pulse profile and polarization are consistent with the predictions of the model.

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