Are pulsars born with a hidden magnetic field?

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Title: Are pulsars born with a hidden magnetic field?
Authors: Torres-Forné, Alejandro | Cerdá-Durán, Pablo | Pons, José A. | Font, José A.
Research Group/s: Astrofísica Relativista
Center, Department or Service: Universidad de Alicante. Departamento de Física Aplicada
Keywords: Stars: magnetic field | Stars: neutron | Pulsars: general
Knowledge Area: Astronomía y Astrofísica
Issue Date: 11-Mar-2016
Publisher: Oxford University Press
Citation: Monthly Notices of the Royal Astronomical Society. 2016, 456(4): 3813-3826. doi:10.1093/mnras/stv2926
Abstract: The observation of several neutron stars in the centre of supernova remnants and with significantly lower values of the dipolar magnetic field than the average radio-pulsar population has motivated a lively debate about their formation and origin, with controversial interpretations. A possible explanation requires the slow rotation of the protoneutron star at birth, which is unable to amplify its magnetic field to typical pulsar levels. An alternative possibility, the hidden magnetic field scenario, considers the accretion of the fallback of the supernova debris on to the neutron star as responsible for the submergence (or screening) of the field and its apparently low value. In this paper, we study under which conditions the magnetic field of a neutron star can be buried into the crust due to an accreting, conducting fluid. For this purpose, we consider a spherically symmetric calculation in general relativity to estimate the balance between the incoming accretion flow and the magnetosphere. Our study analyses several models with different specific entropy, composition, and neutron star masses. The main conclusion of our work is that typical magnetic fields of a few times 1012 G can be buried by accreting only 10−3–10−2 M⊙, a relatively modest amount of mass. In view of this result, the central compact object scenario should not be considered unusual, and we predict that anomalously weak magnetic fields should be common in very young (< few kyr) neutron stars.
Sponsor: This work has been supported by the Spanish MINECO grants AYA2013-40979-P and AYA2013-42184-P and by the Generalitat Valenciana (PROMETEOII-2014-069).
ISSN: 0035-8711 (Print) | 1365-2966 (Online)
DOI: 10.1093/mnras/stv2926
Language: eng
Type: info:eu-repo/semantics/article
Rights: © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Peer Review: si
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Appears in Collections:INV - Astrofísica Relativista - Artículos de Revistas

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