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A Key to Pulsar Wind Bubble Morphologies: Hydrodynamical Simulations

Published online by Cambridge University Press:  19 July 2016

Eric van der Swaluw  and
Turlough P. Downes
Eric van der Swaluw
Affiliation:
FOM-Institute for Plasma Physics Rijnhuizen, P.O. Box 1207, 3430 BE Nieuwegein, The Netherlands
Turlough P. Downes
Affiliation:
School of Mathematical Sciences, Dublin City University, Glasnevin, Dublin 9, Ireland

Abstract

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We present a model of a pulsar-driven supernova remnant, by using a hydrodynamics code, which simulates the evolution of a pulsar wind nebula when the pulsar is moving at a high velocity through its expanding supernova remnant. The simulation shows four different stages of the pulsar wind nebula: the supersonic expansion stage, the reverse shock interaction stage, the subsonic expansion stage and ultimately the bow shock stage. Due to the high velocity of the pulsar, the position of the pulsar is located at the head of the pulsar wind bubble, after the passage of the reverse shock. The resulting morphology of the pulsar wind bubble is therefore similar to the morphology of a bow shock pulsar wind nebulA. We show how to distinguish these two different stages, and apply this method to the SNR G327.1–1.1, for which we argue that there is no bow shock around its pulsar wind nebulA.

Type
Part 4: Pulsar Wind Nebulae and Their Environments
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 175 - 178
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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