Could SXP 1062 be an Accreting Magnetar?

Abstract

In this work we explore the possible evolutionary track of the neutron star in the newly discovered Be/X-ray binary SXP 1062, which is believed to be the first X-ray pulsar associated with a supernova remnant. Although no cyclotron feature has been detected to indicate the strength of the neutron star's magnetic field, we show that it may be $\ga 10^{14} $G. If so SXP 1062 may belong to the accreting magnetars in binary systems. We attempt to reconcile the short age and long spin period of the pulsar taking account of different initial parameters and spin-down mechanisms of the neutron star. Our calculated results show that, to spin down to a period $\sim 1000$s within $10-40$kyr requires efficient propeller mechanisms. In particular, the model for angular momentum loss under energy conservation seems to be ruled out.

19 pages, 4 figures, accepted for publication in ApJ

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• How to make a mature accreting magnetar
• Targeted search for young radio pulsars in the SMC: Discovery of two new pulsars
• Long-term evolution of the neutron-star spin period of SXP 1062
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• The unusual behaviour of the young X-ray pulsar SXP 1062 during the 2019 outburst
• Looking for Hall attractor in astrophysical sources
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• On the formation of the peculiar low-mass X-ray binary IGR J17480$-$2446 in Terzan 5
• The slow X-ray pulsar SXP 1062 and associated supernova remnant in the Wing of the Small Magellanic Cloud
• Study of recently discovered Be/X-ray pulsar MAXI J0655-013 using NuSTAR
• SALT spectroscopy of the HMXB associated with the LMC supernova remnant MCSNR\,J0513$-$6724
• Monte-Carlo simulations on possible collimation effects of outflows to fan-beamed emission of ultraluminous accreting X-ray pulsars
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