Hostname: page-component-78c5997874-8bhkd Total loading time: 0 Render date: 2024-11-08T00:13:28.942Z Has data issue: false hasContentIssue false
  • English
  • Français

Neutron Star Kicks Affected by Standing Accretion Shock Instability for Core-Collapse Supernovae

Published online by Cambridge University Press:  05 September 2012

Wakana Iwakami Nakano ,
Kei Kotake ,
Naofumi Ohnishi ,
Shoichi Yamada  and
Keisuke Sawada
Wakana Iwakami Nakano
Affiliation:
Institute of Fluid Science, Tohoku University, 2-1-1 Katahira, Aoba-ku, Sendai, Miyagi, 980-8577, Japan email: [email protected]
Kei Kotake
Affiliation:
Division of Theoretical Astronomy/Center for Computational Astrophysics, National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan
Naofumi Ohnishi
Affiliation:
Department of Aerospace Engineering, Tohoku University, 6-6-01 Aramaki-Aza-Aoba, Aoba-ku, Sendai, 980-8579, Japan
Shoichi Yamada
Affiliation:
Advanced Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo, 169-8555, Japan
Keisuke Sawada
Affiliation:
Department of Aerospace Engineering, Tohoku University, 6-6-01 Aramaki-Aza-Aoba, Aoba-ku, Sendai, 980-8579, Japan
Rights & Permissions [Opens in a new window]

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.

We investigate a proto-neutron star kick velocity estimated from kinetic momentum of a flow around the proto-neutron star after the standing accretion shock instability grows. In this study, ten different types of random perturbations are imposed on the initial flow for each neutrino luminosity. We found that the kick velocities of proto-neutron star are widely distributed from 40 km s−1 to 180 km s−1 when the shock wave reaches 2000 km away from the center of the star. The average value of kick velocity is 115 km s−1, whose value is smaller than the observational ones. The kick velocities do not depend on the neutrino luminosity.

Keywords

supernovaeshock waveshydrodynamicsinstabilities.
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 337 - 338
Copyright
Copyright © International Astronomical Union 2012

References

Hobbs, G., Lorimer, D. R., Lyne, A. G., & Kramer, M. 2005, MNRAS, 360, 974CrossRefGoogle Scholar
Winkler, P. F. & Petre, R. 2007, ApJ, 670, 635CrossRefGoogle Scholar
Scheck, L., Kifonidis, K., Janka, H.-Th., & Müller, E. 2006, A&A, 457, 963Google Scholar
Nordhaus, J., Brandt, T. D., Burrows, A., Livne, E., & Ott, C. D. 2010, Phys. Rev. D, 82, 103016CrossRefGoogle Scholar
Wongwathanarat, A., Janka, H.-Th., & Müller, E. 2010, ApJ, 725, L106CrossRefGoogle Scholar
Iwakami, W., Kotake, K., Ohnishi, N., Yamada, S., & Sawada, K. 2008, ApJ, 678, 1207CrossRefGoogle Scholar