Astron. Astrophys. 322, 846-856 (1997)

Origin of pulsar radio emission

I. High frequency data

M. Kramer ¹, K.M. Xilouris ², A. Jessner ¹, D.R. Lorimer ¹, R. Wielebinski ¹ and A.G. Lyne <sup>3

1</sup> Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
² National Astronomy and Ionospheric Center, Arecibo Observatory, P.O. Box 995, Arecibo, Puerto Rico 00613
³ University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire, SK11 9DL, UK

Received 20 June 1996 / Accepted 12 December 1996

Abstract

Using the pulse arrival times from pulsar observations made between 1.4 and 32 GHz, we constrain the location and size of the magnetospheric region which is responsible for the observed radio emission. We demonstrate that for long period pulsars the magnetic field maintains its dipolar form throughout the whole emission region. The emission region itself is located very close to the stellar surface and confined to a small slab of a few tens stellar radii in height.

Key words: pulsars: general pulsars: individual: B0329+54, B0355+54, B0540+32, B1133+16, B1706-16, B1929+10, B2020+28, B2021+51 radiation mechanisms: miscellaneous

Send offprint requests to: M. Kramer (mkramer@mpifr-bonn.mpg.de)

SIMBAD Objects

Contents

• 1. Introduction
• 2. Background
• 3. Observations
• 4. Data analysis
  • 4.1. Timing models
  • 4.2. TOA measurements
  • 4.3. Profile alignment
• 5. Results
  • 5.1. PSR B0329+54
  • 5.2. PSR B0355+54
  • 5.3. PSR B0540+23
  • 5.4. PSR B1133+16
  • 5.5. PSR B1706-16
  • 5.6. PSR B1929+10
  • 5.7. PSR B2020+28
  • 5.8. PSR B2021+51
• 6. Discussion
• 7. Conclusion
• Acknowledgements
• References

© European Southern Observatory (ESO) 1997

Online publication: June 5, 1998

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