skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Pulsar Wind Bubble Blowout from a Supernova

Abstract

For pulsars born in supernovae, the expansion of the shocked pulsar wind nebula is initially in the freely expanding ejecta of the supernova. While the nebula is in the inner flat part of the ejecta density profile, the swept-up, accelerating shell is subject to the Rayleigh–Taylor instability. We carried out two- and three-dimensional simulations showing that the instability gives rise to filamentary structure during this initial phase but does not greatly change the dynamics of the expanding shell. The flow is effectively self-similar. If the shell is powered into the outer steep part of the density profile, the shell is subject to a robust Rayleigh–Taylor instability in which the shell is fragmented and the shocked pulsar wind breaks out through the shell. The flow is not self-similar in this phase. For a wind nebula to reach this phase requires that the deposited pulsar energy be greater than the supernova energy, or that the initial pulsar period be in the ms range for a typical 10{sup 51} erg supernova. These conditions are satisfied by some magnetar models for Type I superluminous supernovae. We also consider the Crab Nebula, which may be associated with a low energy supernova for which this scenariomore » applies.« less

Authors:
 [1];  [2]
  1. Department of Physics, North Carolina State University, Raleigh, NC 27695-8202 (United States)
  2. Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States)
Publication Date:
OSTI Identifier:
22663217
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 845; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; CRAB NEBULA; DENSITY; EXPANSION; NEUTRON STARS; PULSARS; RAYLEIGH-TAYLOR INSTABILITY; SIMULATION; STELLAR WINDS; SUPERNOVAE; THREE-DIMENSIONAL CALCULATIONS

Citation Formats

Blondin, John M., and Chevalier, Roger A., E-mail: blondin@ncsu.edu. Pulsar Wind Bubble Blowout from a Supernova. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA8267.
Blondin, John M., & Chevalier, Roger A., E-mail: blondin@ncsu.edu. Pulsar Wind Bubble Blowout from a Supernova. United States. doi:10.3847/1538-4357/AA8267.
Blondin, John M., and Chevalier, Roger A., E-mail: blondin@ncsu.edu. Sun . "Pulsar Wind Bubble Blowout from a Supernova". United States. doi:10.3847/1538-4357/AA8267.
@article{osti_22663217,
title = {Pulsar Wind Bubble Blowout from a Supernova},
author = {Blondin, John M. and Chevalier, Roger A., E-mail: blondin@ncsu.edu},
abstractNote = {For pulsars born in supernovae, the expansion of the shocked pulsar wind nebula is initially in the freely expanding ejecta of the supernova. While the nebula is in the inner flat part of the ejecta density profile, the swept-up, accelerating shell is subject to the Rayleigh–Taylor instability. We carried out two- and three-dimensional simulations showing that the instability gives rise to filamentary structure during this initial phase but does not greatly change the dynamics of the expanding shell. The flow is effectively self-similar. If the shell is powered into the outer steep part of the density profile, the shell is subject to a robust Rayleigh–Taylor instability in which the shell is fragmented and the shocked pulsar wind breaks out through the shell. The flow is not self-similar in this phase. For a wind nebula to reach this phase requires that the deposited pulsar energy be greater than the supernova energy, or that the initial pulsar period be in the ms range for a typical 10{sup 51} erg supernova. These conditions are satisfied by some magnetar models for Type I superluminous supernovae. We also consider the Crab Nebula, which may be associated with a low energy supernova for which this scenario applies.},
doi = {10.3847/1538-4357/AA8267},
journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 845,
place = {United States},
year = {2017},
month = {8}
}