Magnetic Rayleigh-Taylor Instability in Pulsar Wind Nebulae

Details Magnetic Rayleigh-Taylor Instability in Pulsar Wind Nebulae Magnetic Rayleigh-Taylor Instability in Pulsar Wind Nebulae

Nov 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..ses.eb010b&link_type=abstract

American Physical Society, The 70th Annual Meeting of the Southeastern Section, November 6-8, 2003, Wilmington, North Carolina,

Physics

Scientific paper

We present two-dimensional numerical simulations of the development of the Rayleigh-Taylor (RT) instability at the interface between an expanding pulsar wind nebula (PWN) and the swept up shell of supernova ejecta. The simulations include the presence of magnetic field which is supposed to be above equipartition in the PWN, and were done in a proper special relativistic regime. The RT instability in presence of magnetic field is revised in the framework of the PWN expansion, and a stability condition is derived. Simulations show that even a very weak magnetic field can suppress the formation of RT fingers. This has important implications in the correct understanding of the local physical conditions in PWN. This work suggests that efficient radiative cooling in the ejecta shell is required to justify the observed morphology in the Crab Nebula.

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