MHD models of Pulsar Wind Nebulae

Abstract

Pulsar Wind Nebulae (PWNe) are bubbles or relativistic plasma that form when the pulsar wind is confined by the SNR or the ISM. Recent observations have shown a richness of emission features that has driven a renewed interest in the theoretical modeling of these objects. In recent years a MHD paradigm has been developed, capable of reproducing almost all of the observed properties of PWNe, shedding new light on many old issues. Given that PWNe are perhaps the nearest systems where processes related to relativistic dynamics can be investigated with high accuracy, a reliable model of their behavior is paramount for a correct understanding of high energy astrophysics in general. I will review the present status of MHD models: what are the key ingredients, their successes, and open questions that still need further investigation.

18 pages, 5 figures, Invited Review, Proceedings of the "ICREA Workshop on The High-Energy Emission from Pulsars and their Systems", Sant Cugat, Spain, April 12-16, 2010

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• The low frequency radio emission and spectrum of the extended SNR W44: new VLA observations at 74 and 324 MHz
• Deep Chandra Observation of the Pulsar Wind Nebula Powered by the Pulsar J1846-0258 in the Supernova Remnant Kes 75
• Three-dimensional hydrodynamic simulations of asymmetric pulsar wind bow shocks
• Local Kelvin-Helmholtz instability and synchrotron modulation in Pulsar Wind Nebulae

Cited by in corpus (3)

• The population of TeV pulsar wind nebulae in the H.E.S.S. Galactic Plane Survey
• Geminga's puzzling pulsar wind nebula
• TeV Halos are Everywhere: Prospects for New Discoveries