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The non-trivial magnetic configuration in neutron stars

Published online by Cambridge University Press:  27 February 2023

Daniele Viganò Open the ORCID record for Daniele Viganò [Opens in a new window]
Daniele Viganò*
Affiliation:
Institute of Space Sciences (IEEC-CSIC), E-08193 Barcelona, Spain; Institut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, Spain; Institut d’Aplicacions Computacionals de Codi Comunitari (IAC3), Universitat de les Illes Balears, Palma de Mallorca, Baleares E-07122, Spain; email: [email protected]
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Abstract

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While predominantly dipolar, large-scale magnetic fields are usually assumed in most studies involving neutron stars, there are multiple observational, theoretical hints and numerical simulations highlightening the importance of non-dipolar components. I review here the most important observational facts and numerical studies pointing towards the existence of magnetospheric currents and internal small-scale structures, arising from multipoles of poloidal and toroidal fields. This holds for all neutron star stages: at birth, during their lifetime and after a merger.

Keywords

MHDMagnetic fieldsstars: neutronstars: pulsarsgravitationradiation mechanisms: thermal
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 173 - 186
Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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