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Pulsars, formed during supernova explosions, are known to be sources ofrelativistic magnetized winds whose interaction with the expanding supernovaremnants (SNRs) gives rise to a pulsar wind nebula (PWN). We presentspherically symmetric relativistic magnetohydrodynamics (RMHD) simulations ofthe interaction of a pulsar wind with the surrounding SNR, both in particle andmagnetically dominated regimes. As shown by previous simulations, the evolutioncan be divided in three phases: free expansion, a transient phase characterizedby the compression and reverberation of the reverse shock, and a final Sedovexpansion. The evolution of the contact discontinuity between the PWN and theSNR (and consequently of the SNR itself) is almost independent of themagnetization of the nebula as long as the total (magnetic plus particle)energy is the same. However, a different behaviour of the PWN internalstructure is observable during the compression-reverberation phase, dependingon the degree of magnetization=2E The simulations were performed using thethird order conservative scheme by Del Zanna et al. (2003).Comment: 11 pages, Latex, 22 Encapsulated PostScript figures, accepted f or  publication on A&

Spherically symmetric relativistic MHD simulations of pulsar wind nebulae in supernova remnants