Pulsar Wind Nebulae
Mitchell A, Gelfand J (2024)
Publication Type: Book chapter / Article in edited volumes
Publication year: 2024
Publisher: Springer Nature
Edited Volumes: Handbook of X-ray and Gamma-ray Astrophysics
ISBN: 9789811969607
DOI: 10.1007/978-981-19-6960-7_157
Abstract
Pulsar wind nebulae (PWNe), structures powered by energetic pulsars, are known for their detection across the entire electromagnetic spectrum, with diverse morphologies and spectral behavior between these bands. The temporal evolution of the morphology and spectrum of a PWN depends strongly on the properties of the associated neutron star, the relativistic outflow powered by its rotational energy, and surrounding medium, and thereby can vary markedly between objects. Due the continuous, but decreasing, injection of electrons and positrons into the PWN by the pulsar, the brightness and spectral variation within and among their wind nebulae reflect themagnetic field structure and particle transport within the PWN. This can include complex motions such as reverse flows or turbulence due to shock interactions and disruption to the nebula. During the last stage of the PWN’s evolution, when the neutron star moves supersonically with respect to its environment, the escape of accelerated particles into the surrounding medium creates an extensive halo evident in very-high-energy gamma-rays. This chapter describes some of the identifying characteristics and key aspects of pulsar wind nebulae through their several evolutionary stages.
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United Arab Emirates (AE)How to cite
APA:
Mitchell, A., & Gelfand, J. (2024). Pulsar Wind Nebulae. In Cosimo Bambi, Andrea Santangelo (Eds.), Handbook of X-ray and Gamma-ray Astrophysics. Springer Nature.
MLA:
Mitchell, Alison, and J. Gelfand. "Pulsar Wind Nebulae." Handbook of X-ray and Gamma-ray Astrophysics. Ed. Cosimo Bambi, Andrea Santangelo, Springer Nature, 2024.
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