An inverse Compton scattering (ICS) model of pulsar emission

2)((1)Department of Geophysics; China (2) Beijing Astronomical Observatory; Chinese Academy of Sciences); G.J.Qiao (1); Peking University; W.P.Lin (1

An inverse Compton scattering (ICS) model of pulsar emission

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arxiv astro-ph/9708245 v1 pith:RVNXJOYJ submitted 1997-08-27 astro-ph

G.J.Qiao (1) , W.P.Lin (1 , 2)((1)Department of Geophysics , Peking University , China (2) Beijing Astronomical Observatory , Chinese Academy of Sciences) This is my paper · ORCID

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Core and conal emission beams of radio pulsars have been identified observationally (Rankin 1983,1993; 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 to be produced and 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 presented a development of 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 adopted and which is adequate to explain pulsar radiation. The theoretical results are in agreement with observations very well.

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On the Fast-radio-burst-associated X-ray Bursts: Inverse Compton Scattering of Radio Photons by an Extreme Pair Flow During Magnetosphere Activities
astro-ph.HE 2025-07 conditional novelty 6.0 of 10

The hard, time-shifted X-ray peaks associated with FRB 200428 and FRB 221014 can be explained by inverse Compton scattering of FRB photons by an extreme pair flow near the light cylinder.

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