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Erratum: Magnetic coupling of planets and small bodies with a pulsar wind.

Abstract : Aims. This paper investigates the electromagnetic interaction of a relativistic stellar wind with a planet or a smaller body in orbit around the neutron star. The interaction is based on the theory of Alfvén wings adapted to the context of relativistic winds.The 2011 paper comprises a short section with numerical applications. This requires an estimate of the magnetic field in the pulsar wind, that depend on the magnetic flux Ψ in the wind asymptotic regime. This flux is badly approximated. Methods. The present erratum corrects the consequences of this wrong estimate of Ψ in three papers where it has consequences: about the magnetic drag acting on pulsar companions, and a model of fast radio bursts (FRB). Results. In those three papers, the physics is unchanged, but the numerical results must be re-scaled. The theory of FRB published in 2014 is briefly discussed.1. Magnetic coupling of planets and small bodies with a pulsar wind In Mottez & Heyvaerts (2011b), the magnetic field in the pulsar wind is expressed as a function of the magnetic flux in the asymptotic regime of the wind Ψ = B r 0 r 2 , where B r 0 is the local magnetic field, and r is the distance to the neutron star. This is an integral of motion along stream lines. In the end of section 2, in view of numerical applications , it is evaluated as Ψ = B r * R 2 * where quantities with a star refer to the neutron star (NS) surface. This approximation corresponds to the monopole solution, which overestimates the wind magnetic field by orders of magnitude. Because this is an asymptotic approximation, its value must be evaluated in the domain where the field lines are wind-like, not on the NS surface. The most admitted approximation is its value at the light cylinder Goldreich & Julian (1969), where between the NS surface and the light cylinder (LC), the magnetic field is supposed dipo-lar. Then, Ψ = B r LC r 2 LC = B * R 3 * Ω * /c where Ω is the NS angular velocity, and c is the speed of light. Then the toroidal component of the pulsar wind magnetic field is approximated by B φ 0 = B * R 3 * Ω 2 * /rc 2 where r >> r LC. ⋆ Deceased.
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Contributor : Fabrice Mottez Connect in order to contact the contributor
Submitted on : Monday, May 11, 2020 - 11:27:20 AM
Last modification on : Wednesday, November 17, 2021 - 12:27:18 PM


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Fabrice Mottez, J Heyvaerts. Erratum: Magnetic coupling of planets and small bodies with a pulsar wind.. Astronomy and Astrophysics - A&A, EDP Sciences, 2020. ⟨hal-02569291⟩



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