Hostname: page-component-76fb5796d-9pm4c Total loading time: 0 Render date: 2024-04-26T23:51:00.182Z Has data issue: false hasContentIssue false
  • English
  • Français

A VLBI Search for a Pulsar Nebula in SN1993J in the Galaxy M81

Published online by Cambridge University Press:  12 April 2016

N. Bartel ,
M. F. Bietenholz ,
W. H. Cannon ,
M. P. Rupen ,
A. J. Beasley ,
D. A. Graham ,
V. I. Altunin ,
T. Venturi ,
G. Umana  and
J. E. Conway
N. Bartel
Affiliation:
York University, Toronto, ONT M3J 1P3, Canada
M. F. Bietenholz
Affiliation:
York University, Toronto, ONT M3J 1P3, Canada
W. H. Cannon
Affiliation:
York University, Toronto, ONT M3J 1P3, Canada
M. P. Rupen
Affiliation:
National Radio Astronomy Observatory, Socorro, NM 87801, U.S.A.
A. J. Beasley
Affiliation:
National Radio Astronomy Observatory, Socorro, NM 87801, U.S.A.
D. A. Graham
Affiliation:
Max-Planck-Institut für Radioastronomie, Postfach 2024, 53010 Bonn, Germany
V. I. Altunin
Affiliation:
Jet Propulsion Laboratory, Pasadena, CA 91009, U.S.A.
T. Venturi
Affiliation:
Istituto di Radioastronomia, 40129 Bologna and 96017 Noto, Italy
G. Umana
Affiliation:
Istituto di Radioastronomia, 40129 Bologna and 96017 Noto, Italy
J. E. Conway
Affiliation:
Onsala Space Observatory, Onsala, Sweden

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.

Twenty consecutive VLBI images of supernova 1993J in M81 from the time of explosion to the present show the dynamic evolution of the expanding radio shell of an exploded star. No clear sign of a pulsar nebula, expected to have a spectral luminosity 10 to 1,000 times larger than that of the Crab, has yet been seen. The upper limit on the brightness at 8.4 GHz in the center of the shell in one of the latest images is 0.15 mJy per beam of 0.4 mas2, corresponding to a spectral luminosity of that of the Crab. Any nebula that may have formed in the center is probably still obscured by the surrounding thermal matter with no substantial filamentation having yet occurred in the latter.

Type
Part 7. The Surrounding of Pulsars
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 515 - 516
Copyright
Copyright © Astronomical Society of the Pacific 2000

References

Bandiera, R., Padni, F., & Salvati, M., 1984, ApJ, 285, 134 CrossRefGoogle Scholar
Bartel, N. et al. 2000, Science, 287, 112 Google Scholar
Bietenholz, M.F., Bartel, N., & Rupen, M.P. 2000, ApJ, in pressGoogle Scholar
Bietenholz, M.F., Kronberg, P.P., Hogg, D.E., & Wilson, A.S. 1991, ApJ, 373, L59 Google Scholar
Chevalier, R.A. 1982, ApJ, 258, 790 Google Scholar
Reynolds, S.P. & Chevalier, R.A. 1984, ApJ, 278, 630 Google Scholar