Hostname: page-component-78c5997874-dh8gc Total loading time: 0 Render date: 2024-11-06T08:15:00.007Z Has data issue: false hasContentIssue false
  • English
  • Français

Asymmetric Supernova Explosions: The Origin of Runaway Pulsars and Binary Pulsars

Published online by Cambridge University Press:  14 August 2015

Jean-Pierre De Cuyper
Jean-Pierre De Cuyper*
Affiliation:
Astrofysisch Instituut, Vrije Universiteit Brussel, Belgium

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.

It is known from observations that pulsars are high velocity objects. As a sizable fraction of these collapsars originates from low velocity single stars, they must have received a “kick” velocity at their birth. Which we assume to be due to the asymmetry of the SN-explosion and to be randomly orientated. Hanson (1979) estimated this asymmetric velocity in a statistical study to be about 102 km s−1. For SNe occurring in binaries the runaway velocities depend on the initial conditions. According to hydrodynamical calculations by Fryxell and Arnett (1979) the momentum imparted by the SN shell to the companion is some 80% of the momentum incident on the geometric cross-section of the star. This is due to mass stripping, which reduces the radius of stars with extended atmospheres, and to a smooth flow of the SN shell around the spherical companion and the nearly spherically symmetric ablation of some mixed stellar material. The mass loss of the companion is negligible.

Type
IX. Pulsars and Supernovae
Information
Symposium - International Astronomical Union , Volume 95: Pulsars , 1981 , pp. 399 - 401
Copyright
Copyright © Reidel 1981 

References

Fryxell, B. A. and Arnett, W. D.: 1979, Enrico Fermi Inst. Preprint N° 78–64.Google Scholar
Hanson, R. B.: 1979, Mon. Not. R. Astr. Soc. 186, p. 357.CrossRefGoogle Scholar
Helfand, D. J., Taylor, J. H., Backus, P. R., and Cordes, J. M.: 1980, Astrophys. J. 237, p. 206.CrossRefGoogle Scholar
Taylor, J. H.: 1981, this volume.Google Scholar
Stone, R. C.: 1979, Astrophys. J. 232, p. 520.CrossRefGoogle Scholar