The Crab nebula in the light of three-dimensional relativistic MHD simulations

Pulsar wind nebulae inside young supernova remnants, and in particular the Crab nebula, are probably the best laboratories for high-energy astrophysics and relativistic plasma physics. They have been modeled numerically for more than a decade through multi-dimensional relativistic MHD simulations, relying on axial symmetry until a few years ago while currently using full three-dimensional simulations employing adaptive meshes. Here, we discuss the most recent findings, especially those obtained by our Arcetri group, focusing on the problem of magnetic field dissipation inside the nebula.

Volume

30

Issue

S1

Start page

93

Uri

http://hdl.handle.net/20.500.12386/29482

Url

https://link.springer.com/article/10.1007/s12210-019-00759-y

Issn Identifier

2037-4631

Ads BibCode

https://ui.adsabs.harvard.edu/abs/2019RLSFN.tmp....1D/abstract

Rights

open.access

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The Crab nebula in the light of three-dimensional relativistic MHD simulations

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