2006/08/11 by N. Bucciantini, Bucciantini, N.
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0608258
6 pages, 6 figures Proceedings of the 1st IGPP-Calspace Conference "Numerical Modeling of Space Plasma Flows", 26-30 March 2006, Palm Springs, CA
arxiv created 2006/08/11 · arxiv updated 2009/12/01
The recent development of numerical schemes for Relativistic MHD (RMHD) allows us to model the acceleration and outflow properties of winds from compact sources. Theoretical models suggest that acceleration and collimation of the flow are extremely inefficient when the speed is close to c, in contrast with many observations. Numerical results for an axisymmetric rotator, both in the case of monopolar and dipolar magnetic field will be presented, suggesting that in ideal RMHD acceleration is indeed inefficient. I will also mention numerical challenges and stability problems of present simulations. Finally I will discuss the interaction of a pulsar wind with the surrounding SNR. I will present emission maps based on numerical simulations of the flow inside the nebula and how they can be used in comparison with observations to derive informations about the properties of pulsar winds far away from the source.