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Astron. Astrophys. 333, 172-180 (1998)

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An inverse Compton scattering (ICS) model of pulsar emission

I. Core and conal emission beams

G.J. Qiao 1 and W.P. Lin 1, 2

1 Department of Geophysics, Peking University, Beijing 100871, P.R. China (gjn@pku.edu.cn)
2 Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, P.R. China (linwp@qso.bao.ac.cn)

Received 18 July 1996 / Accepted 5 December 1997


Core and conal emission beams of radio pulsars have been identified observationally (Rankin 1983, 1993a, b; Lyne and Manchester 1988). In the inner gap model (Ruderman and Sutherland 1975, hereafter RS75), the gap continually breaks down (sparking) by forming electron-positron pairs on a time scale of a few microseconds (RS75). This makes a large amplitude low frequency wave which would be scattered by relativistic particles moving out from the gap. Under this assumption, Qiao (1988a, 1992) presented an Inverse Compton Scattering (ICS) model for both core and conal emissions. This paper develops the model. Retardation and aberration effects due to different radiation components emitted from different heights are considered. The luminosity of pulsar radio emission via the ICS process is discussed. Coherent emission by bunches of particles is adequate to explain pulsar radiation. The theoretical results agree with observations very well.

Key words: pulsars: general – radiation mechanisms: non-thermal

Send offprint requests to: G.J. Qiao

© European Southern Observatory (ESO) 1998

Online publication: April 15, 1998