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Stochastic spin evolution of neutron stars

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arxiv astro-ph/0110022 v1 pith:QPARZYQV submitted 2001-10-01 astro-ph

S.B. Popov (1) , M.E. Prokhorov (1) , A.V. Khoperskov (2) , V.M. Lipunov (1 , 3) ((1) Sternberg Astronomical Institute , (2) Volgograd State University , (3) Moscow State University , Department of Physics) This is my paper · ORCID
classification astro-ph
keywords inssspinevolutionaccretedcalculationslongmagneticmomentum
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abstract

In this paper we present calculations of period distribution for old accreting isolated neutron stars (INSs). At the age about a few billions years low velocity INSs come to the stage of accretion. At that stage their period evolution is governed by magnetic breaking and accreted angular momentum. Due to turbulence of the interstellar medium (ISM) accreted momentum can both accelerate and decelerate rotation of an INS and spin evolution has chaotic character. Calculations show that for constant magnetic fields INSs have relatively long spin periods, $\ge 10^4$--$10^5$ s, depending on parameters of INSs and an ISM. Due to long periods INSs have high spin up/spin down rates, which should fluctuate on a time scale about a few years.

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  1. A binary origin of ultra-long period radio pulsars

    astro-ph.HE 2025-07 conditional novelty 6.0 of 10

    Wind-fed accretion in wide massive binaries can spin neutron stars down past 1000 s, and supernova disruption of the binary then leaves isolated ultra-long period pulsars at a rate of about 10^-6 per year.

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