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MHD models of Pulsar Wind Nebulae

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High-Energy Emission from Pulsars and their Systems

Part of the book series: Astrophysics and Space Science Proceedings ((ASSSP))

Abstract

PulsarWind 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.

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  1. NORDITA, Roslagstullsbacken 23, 106 91, Stockholm, Sweden

    Niccolò Bucciantini

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  1. Niccolò Bucciantini
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Correspondence to Niccolò Bucciantini .

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  1. Inst. Ciències de l'Espai, CSIC Bellaterra, Campus UAB, Bellaterra, 08193, Spain

    Diego F. Torres

  2. Inst. Ciències de l'Espai, CSIC Bellaterra, Campus UAB, Bellaterra, 08193, Spain

    Nanda Rea

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Bucciantini, N. (2011). MHD models of Pulsar Wind Nebulae. In: Torres, D., Rea, N. (eds) High-Energy Emission from Pulsars and their Systems. Astrophysics and Space Science Proceedings. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-17251-9_39

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  • DOI: https://doi.org/10.1007/978-3-642-17251-9_39

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