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

Details The Vector Model of Pulsar Emission: Observations in i the UV and Visible The Vector Model of Pulsar Emission: Observations in i the UV and Visible

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.5002d&link_type=abstract

American Astronomical Society, 192nd AAS Meeting, #50.02; Bulletin of the American Astronomical Society, Vol. 30, p.886

Astronomy and Astrophysics

Astronomy

Scientific paper

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 & 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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