Probing the neutron star spin evolution in the young Small Magellanic Cloud Be/X-ray binary SXP 1062

Authors

  • S. B. Popov,

    Corresponding author
    1. Sternberg Astronomical Institute, Moscow State University, 119992 Moscow, Russia
    2. Dipartimento di Fisica e Astronomia, Università di Padova, via Marzolo 8, I-35131 Padova, Italy
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  • R. Turolla

    1. Dipartimento di Fisica e Astronomia, Università di Padova, via Marzolo 8, I-35131 Padova, Italy
    2. Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT
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E-mail: sergepolar@gmail.com

ABSTRACT

The newly discovered Be/X-ray binary in the Small Magellanic Cloud, SXP 1062, provides the first example of a robust association with a supernova remnant (SNR). The short age estimated for the SNR qualifies SXP 1062 as the youngest known source in its class, inline image. As such, it allows us to test current models of magnetorotational evolution of neutron stars in a still unexplored regime. Here we discuss possible evolutionary scenarios for SXP 1062 in an attempt to reconcile its long spin period, inline image, and short age. Although several options can be considered, like an anomalously long initial period or the presence of a fossil disc, our results indicate that SXP 1062 may host a neutron star born with a large initial magnetic field, typically in excess of ∼ 1014  G, which then decayed to ∼ 1013  G.

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