Volume 377, Number 3, October III 2001
|Page(s)||964 - 971|
|Section||Interstellar and circumstellar matter|
|Published online||15 October 2001|
An inverse Compton scattering (ICS) model of pulsar emission
II. Frequency behavior of pulse profiles
Astronomy Department, Peking University, Beijing 100871, PR China
2 Chinese Academy of Science -Peking University Joint Beijing Astrophysics Center, Beijing 100871, PR China
3 : Astronomy & Astrophysics Department, Pennsylvania State University, University Park, PA 16802, USA
4 National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR China
Corresponding author: G. J. Qiao, firstname.lastname@example.org
Accepted: 9 August 2001
The shapes of pulse profiles, especially their variations with respect to observing frequencies, are very important to understand emission mechanisms of pulsars. However, no previous attempt has been made to interpret their complicated phenomenology. In this paper, we present theoretical simulations for the integrated pulse profiles and their frequency evolution within the framework of the inverse Compton scattering (ICS) model proposed by Qiao ([CITE]) and Qiao & Lin ([CITE]). Using the phase positions of the pulse components predicted by the "beam-frequency figure" of the ICS model, we present Gaussian fits to the multi-frequency pulse profiles for some pulsars. It is shown that the model can reproduce various types of the frequency evolution behaviors of pulse profiles observed.
Key words: stars: pulsars: general / radiation mechanisms: non-thermal
© ESO, 2001
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