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On the nature of optical emission from radio pulsars

Published online by Cambridge University Press:  12 April 2016

I.F. Malov  and
G.Z. Machabeli
I.F. Malov
Affiliation:
Pushchmo Radio Astronomy Observatory, Lebedev Physical Institute, 142292, Pushchmo, Russia
G.Z. Machabeli
Affiliation:
Pushchmo Radio Astronomy Observatory, Lebedev Physical Institute, 142292, Pushchmo, Russia

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There are more than one thousand known radio pulsars, but only 9 of them have detected optical emission (Caraveo 1999). A part of optical emission can be caused by thermal radiation from the hot surface of the neutron star. We shall try to describe the non-thermal component (Kurt et al. 1980) on the base of the synchrotron mechanism, using one-dimensional distribution function of emitting electrons.

One of the possible reasons of observed pulsar emission is the cyclotron instability developed in an anisotropic plasma (Sagdeev & Shafranov 1960). To generate transversal (t) waves with the spectrum

the condition of the cyclotron resonance (Kazbegi et al. 1992)

must be fulfilled. Here is the Lorentz-factor of resonance particles, is the drift velocity of particles, ρ is the curvature radius of field lines.

Type
Part 6. Emission and Plasma Theory
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 421 - 422
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Caraveo, P.A. these proceedingsGoogle Scholar
Kurt, V.G., Sokolov, V.V., Zharikov, S.A. et al. 1980, A&A 301, 547 Google Scholar
Sagdeev, R.Z., Shafranov, V.D. 1960, Zh. Exp.Theor.Phys., 39, 181 Google Scholar
Kazbegi, A.Z., Machabeli, G.Z., Melikidze, G.I. Proc IAU Colloq. 128. 1992. P.232.Google Scholar
Epstein, R.I. 1973, ApJ 183, 593 Google Scholar