Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-23T16:34:10.476Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Case for Magnetic Field Line Sweep-Back in Pulsars 0950+08 and 1133+16

Published online by Cambridge University Press:  27 September 2017

T. H. Hankins ,
V. A. Izvekova ,
V. M. Malofeev ,
J. M. Rankin ,
Yu. P. Shitov  and
D. R. Stinebring
T. H. Hankins
Affiliation:
Very Large Array, National Radio Astronomy Observatory and Department of Physics, New Mexico Institute of Mining and Technology
V. A. Izvekova
Affiliation:
Radio Astronomy Department, Lebedev Physical Institute
V. M. Malofeev
Affiliation:
Radio Astronomy Department, Lebedev Physical Institute
J. M. Rankin
Affiliation:
Department of Physics, University of Vermont
Yu. P. Shitov
Affiliation:
Radio Astronomy Department, Lebedev Physical Institute
D. R. Stinebring
Affiliation:
Department of Physics, Oberlin College

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Coordinated profile observations between 25 MHz and 5 GHz have been carried out at the Arecibo and Pushchino observatories, and aligned according to dispersion measure (DM) values determined by cross-correlating microstructure features at adjacent frequencies. The average profiles of the nearly aligned rotator PSR 0950+08 align satisfactorily using the DM value of 2.9701 pc cm–3. For PSR 1133+16 excess delay at low frequencies is observed when alignment is made using the value of DM = 4.8413 pc cm–3 determined from microstructure cross-correlations

Type
Part I Structure of the magnetic field
Information
International Astronomical Union Colloquium , Volume 128: Magnetospheric structure and emission mechanisms of radio pulsars , 1992 , pp. 9 - 10
Copyright
Copyright © United States Naval Observatory 1992