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Intensity Dependence of the PSR 0329+54 Pulse Profile

Published online by Cambridge University Press:  27 September 2017

M. M. McKinnon  and
T. H. Hankins
M. M. McKinnon
Affiliation:
Very Large Array, National Radio Astronomy Observatory and Department of Physics, New Mexico Institute of Mining and Technology
T. H. Hankins
Affiliation:
Very Large Array, National Radio Astronomy Observatory and Department of Physics, New Mexico Institute of Mining and Technology

Abstract

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Following the analysis by Krishnamohan and Downs (1983) of the Vela pulsar, we have investigated the behavior of the core and outrider components of PSR 0329+54 by calculating pulse profiles at different pulse intensities. VLA observations of individual pulses from PSR 0329+54 at 1415 MHz were used in our analysis. Our investigation reveals the following dependencies upon increasing core peak intensity:

  1. (i) earlier core arrival times,

  2. (ii) decreasing separation of the left outrider relative to the core,

  3. (iii) increasing separation of the right outrider relative to the core,

  4. (iv) decreasing outrider-to-core peak intensity ratios, and

  5. (v) essentially constant core width.

To explain these dependencies, we propose a simple model in which the location of the core centroid is altered near the neutron star surface. The model and data are consistent with the mode-switching signatures and magnetospheric absorption features known to exist in this pulsar.

Type
Part IV Form and spectra of emission beams
Information
International Astronomical Union Colloquium , Volume 128: Magnetospheric structure and emission mechanisms of radio pulsars , 1992 , pp. 190 - 192
Copyright
Copyright © United States Naval Observatory 1992