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

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

2003-03-21

arxiv.org/abs/astro-ph/0303491v1

Astron.Astrophys. 405 (2003) 617-626

Astronomy and Astrophysics

Astrophysics

11 pages, Latex, 22 Encapsulated PostScript figures, accepted f or publication on A&A

Scientific paper

10.1051/0004-6361:20030624

Pulsars, formed during supernova explosions, are known to be sources of relativistic magnetized winds whose interaction with the expanding supernova remnants (SNRs) gives rise to a pulsar wind nebula (PWN). We present spherically symmetric relativistic magnetohydrodynamics (RMHD) simulations of the interaction of a pulsar wind with the surrounding SNR, both in particle and magnetically dominated regimes. As shown by previous simulations, the evolution can be divided in three phases: free expansion, a transient phase characterized by the compression and reverberation of the reverse shock, and a final Sedov expansion. The evolution of the contact discontinuity between the PWN and the SNR (and consequently of the SNR itself) is almost independent of the magnetization of the nebula as long as the total (magnetic plus particle) energy is the same. However, a different behaviour of the PWN internal structure is observable during the compression-reverberation phase, depending on the degree of magnetization=2E The simulations were performed using the third order conservative scheme by Del Zanna et al. (2003).

Affiliated with

Also associated with

No associations

Rating

Spherically symmetric relativistic MHD simulations of pulsar wind nebulae in supernova remnants does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Spherically symmetric relativistic MHD simulations of pulsar wind nebulae in supernova remnants, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Spherically symmetric relativistic MHD simulations of pulsar wind nebulae in supernova remnants will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-153686