Hostname: page-component-6bf8c574d5-86b6f Total loading time: 0 Render date: 2025-03-07T12:37:45.305Z Has data issue: false hasContentIssue false
  • English
  • Français

The Polarization of the Crab Pulsar with HST

Published online by Cambridge University Press:  12 April 2016

Joseph F. Dolan ,
Patricia T. Boyd ,
Robert J. Hill ,
F. Graham-Smith ,
A. G. Lyne ,
James D. Biggs ,
J. W. Percival ,
Edward L. Robinson  and
G. Wayne van Citters
Joseph F. Dolan
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771
Patricia T. Boyd*
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771
Robert J. Hill*
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771
F. Graham-Smith
Affiliation:
University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire SK119DL, UK
A. G. Lyne
Affiliation:
University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire SK119DL, UK
James D. Biggs
Affiliation:
Perth Observatory, Walnut Road, Bickley 6076, Western Australia
J. W. Percival
Affiliation:
Department of Astronomy and Space Astronomy Laboratory, University of Wisconsin, Madison, WI 53706
Edward L. Robinson
Affiliation:
Department of Astronomy and McDonald Observatory, University of Texas, Austin, TX 78712
G. Wayne van Citters
Affiliation:
Division of Astronomical Sciences, National Science Foundation, 4201 Wilson Blvd., Arlington, VA 22230
*
*also Universities Space Research Association
†also Hughes STX Corporation

Extract

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.

The linear polarization of the Crab pulsar as a function of pulse phase was observed by the High Speed Photometer on the Hubble Space Telescope in March, 1993. Observations were obtained in a bandpass centered on 2770 A using a 0.25 ms sample time, corresponding to a time resolution of 0.0075 in pulse phase. The UV polarization of the pulsar [Fig. 1] is strikingly similar to that observed in the visible (cf. Smith et al. 1988). The same values of polarization and the same swing of position angle occur through the main and secondary pulses. The polarization pulse profile must be essentially wavelength independent at frequencies above the infrared.

Type
Part 5 High Energy Phenomena
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 301 - 302
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

Percival, J.W. et at., 1993, ApJ, 407, 276.CrossRefGoogle Scholar
Smith, F.G., Jones, D.H.P., Dick, J.S.B. & Pike, C.D., 1988 MNRAS, 233, 305.CrossRefGoogle Scholar
Wardle, J.F.C. & Kronberg, P.P. 1974, ApJ, 255, L1.Google Scholar