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A low energy-model for coherent radio emission — the three-liter-pulsar

Published online by Cambridge University Press:  12 April 2016

Harald Lesch ,
Thomas Kunzl  and
Axel Jessner
Harald Lesch
Affiliation:
University Observatory, Scheinerstr. 1, 81679 Munich, Germany
Thomas Kunzl
Affiliation:
University Observatory, Scheinerstr. 1, 81679 Munich, GermanyMax-Planck-Institut for Extraterrestrial Physics, Giessenbachstr., 85748 Garching, Germany
Axel Jessner
Affiliation:
Max-Planck-Institut for Radioastronomy, Auf dem Hügel 69, 53121 Bonn, Germany

Abstract

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We present a new model for the coherent radio emission of pulsars that succeeds in reproducing observed luminosities at emission heights of 50-100 pulsar radii. Based on energy conservation and propagation effects we apply the concept of a free electron maser (FEM) to the creation of coherent radio emission. With the characteristic frequency ν ≃ γ2νpe (νpe denotes the plasma frequency and γ is the Lorentz factor of the emitting particles) we find that even for the lowest frequencies at which the highest degree of coherence is required only low energy particles (γ ≃ 10) with Goldreich-Julian-density are necessary. Because of its low energy budget we call it three-liter-pulsar.

Type
Part 6. Emission and Plasma Theory
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 381 - 386
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Asseo, E. 1993, MNRAS, 264, 940 CrossRefGoogle Scholar
Goldreich, P., & Julian, W.H. 1969, ApJ 157, 869 CrossRefGoogle Scholar
Kijak, J., & Gil, J.A. 1998, MNRAS 299, 855 CrossRefGoogle Scholar
Kramer, M., et al. 1997, A&A, 322, 846 Google Scholar
Kuijpers, J., & Volwerk, M. 1996, ASP-Series 105, 181 Google Scholar
Kunzl, T., Lesch, H., & Jessner, A. 1998a, A&A, 339, 917 Google Scholar
Kunzl, T., Lesch, H., Jessner, A., & von Hoensbroech, A. 1998b, ApJ, 505, L139 CrossRefGoogle Scholar
Kunzl, T., Lesch, H., & Jessner, A. 1999, ApJ (submitted)Google Scholar
Lange, C., Kramer, M., Wielebinski, R., & Jessner, A. 1998, A&A, 332, 111 Google Scholar
Lesch, H., Jessner, A., Kramer, M., & Kunzl, T. 1998, A&A, 332, L21 Google Scholar
Malofeev, V.M., et al. 1994, A&A 285, 201 Google Scholar
Melrose, D.B. 1995, J.Astrophys. Astron., 16, 137 CrossRefGoogle Scholar
Melrose, D.B., & Gedalin, M.E., 1999, ApJ, 521, 351 CrossRefGoogle Scholar
Usov, V.V. 1987, ApJ 320, 333 CrossRefGoogle Scholar