Volume 412, Number 2, December III 2003
|Page(s)||473 - 479|
|Section||Stellar structure and evolution|
|Published online||28 November 2003|
Refraction in a pulsar magnetosphere – the effect of a variable emission height on pulse morphology
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
2 Stichting ASTRON, Postbus 2, 7990 AA Dwingeloo, The Netherlands
3 Institute for Theoretical Physics, University of Amsterdam, Valckenierstraat 65, 1018 XE Amsterdam, The Netherlands
Corresponding author: P. Weltevrede, email@example.com
Accepted: 15 September 2003
The [CITE] model to calculate pulse profiles is extended to a variable emission height model to make it physically self-consistent. In this context variable means that the emission height is no longer considered to be the same for different magnetic field lines. The pulse profiles calculated using this new model seem to be less realistic due to a focusing effect and cannot be used to fit (typical) multifrequency pulsar observations. Apart from the focusing effect the general morphology of pulse profiles is not greatly affected by introducing a variable emission height. Additional extensions of the model will be needed to be able to fit observations, and several suggestions are made.
Key words: plasmas / waves / stars: pulsars general
© ESO, 2003
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