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Evolution of neutron star magnetic fields

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arxiv 2109.05584 v1 pith:XHVEK7GN submitted 2021-09-12 astro-ph.HE

Andrei P. Igoshev , Sergei B. Popov , Rainer Hollerbach This is my paper · ORCID
classification astro-ph.HE
keywords neutronfieldmagneticstarsevolutionfieldsstarcompact
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Neutron stars are natural physical laboratories allowing us to study a plethora of phenomena in extreme conditions. In particular, these compact objects can have very strong magnetic fields with non-trivial origin and evolution. In many respects its magnetic field determines the appearance of a neutron star. Thus, understanding the field properties is important for interpretation of observational data. Complementing this, observations of diverse kinds of neutron stars enable us to probe parameters of electro-dynamical processes at scales unavailable in terrestrial laboratories. In this review we first briefly describe theoretical models of formation and evolution of magnetic field of neutron stars, paying special attention to field decay processes. Then we present important observational results related to field properties of different types of compact objects: magnetars, cooling neutron stars, radio pulsars, sources in binary systems. After that, we discuss which observations can shed light on obscure characteristics of neutron star magnetic fields and their behaviour. We end the review with a subjective list of open problems.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Screening rho-meson mass in the presence of strong magnetic fields

    hep-ph 2025-02 reject novelty 6.0 of 10

    The paper claims a first calculation of the rho-meson screening mass in strong magnetic fields, with two modes increasing with eB and one mode nearly constant.

  2. On Ultra-long Period (53.8 min) Pulsar ASKAP J1935+2148: Coherent Radio Emission Triggered by Local Superstrong Magnetic Reconnection

    astro-ph.HE 2025-08 conditional novelty 5.0 of 10

    Ultra-long period pulsars may be Crab-like pulsars spun down by particle winds, with their radio emission powered by local magnetic reconnection instead of rotation.

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