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Pulsar Striped Winds

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Modelling Pulsar Wind Nebulae

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 446))

Abstract

According to magnetohydrodynamic (MHD) models, the rotational energy of a rapidly spinning neutron star is carried away by a relativistic wind and deposited at a large distance, in the nebula, downstream of the wind termination shock. The energy transport in the outflow is mediated by Poynting flux, but it is not clear how the energy stored in the fields is transferred into the energized population of emitting particles. The most plausible dissipation mechanisms are thought to be related to the “striped” structure of the wind, in particular, to the existence of a current sheet, prone to reconnection events. In this model the current sheet is a natural place for internal dissipation and acceleration of particles responsible for pulsed, high-energy emission. Moreover, reconnection is a promising scenario for explaining annihilation of fields at the shock and conversion of their energy into the kinetic energy of particles. The shock structure, however, is likely to differ in the low-density plasmas, in which non-MHD effects intervene. In this regime, the striped wind can dissipate its energy via an electromagnetic precursor of the shock.

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Acknowledgements

I thank Tomasz Rembiasz and Jérôme Pétri for helpful comments on the manuscript.

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  1. Observatoire Astronomique de Strasbourg, 11 Rue de l’Université, F-67000, Strasbourg, France

    Iwona Mochol

  2. Institute of Nuclear Physics, Polish Academy of Sciences, ul. E. Radzikowskiego 152, 31-342, Kraków, Poland

    Iwona Mochol

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  1. ICREA & Institute of Space Sciences, (IEEC-CSIC) Campus UAB, Barcelona, Spain

    Diego F. Torres

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Mochol, I. (2017). Pulsar Striped Winds. In: Torres, D. (eds) Modelling Pulsar Wind Nebulae. Astrophysics and Space Science Library, vol 446. Springer, Cham. https://doi.org/10.1007/978-3-319-63031-1_7

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