Volume 637, May 2020
|Number of page(s)||6|
|Section||Stellar structure and evolution|
|Published online||08 May 2020|
The unusual behavior of the young X-ray pulsar SXP 1062 during the 2019 outburst
Department of Physics and Astronomy, University of Turku, 20014 Turku, Finland
2 Space Research Institute of the Russian Academy of Sciences, Profsoyuznaya Str. 84/32, Moscow 117997, Russia
3 Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, 72076 Tübingen, Germany
4 Leiden Observatory, Leiden University, 2300 RA Leiden, The Netherlands
5 Pulkovo Observatory, Russian Academy of Sciences, Saint Petersburg 196140, Russia
6 Max-Planck-Institut für Extraterrestrische Physik, Gießenbachstraße, 85748 Garching, Germany
7 Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA
8 Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, 10691 Stockholm, Sweden
Accepted: 24 March 2020
We present the results of the first dedicated observation of the young X-ray pulsar SXP 1062 in the broad X-ray energy band obtained during its 2019 outburst with the NuSTAR and XMM-Newton observatories. The analysis of the pulse-phase averaged and phase-resolved spectra in the energy band from 0.5 to 70 keV did not reveal any evidence for the presence of a cyclotron line. The spin period of the pulsar was found to have decreased to 979.48 ± 0.06 s implying a ∼10% reduction compared to the last measured period during the monitoring campaign conducted about five years ago, and is puzzling considering that the system apparently has not shown major outbursts ever since. The switch of the pulsar to the spin-up regime supports the common assumption that torques acting on the accreting neutron star are nearly balanced and thus SXP 1062 likely also spins with a period close to the equilibrium value for this system. The current monitoring of the source also revealed a sharp drop in its soft X-ray flux right after the outburst, which is in drastic contrast to the behavior during the previous outburst when the pulsar remained observable for years with only a minor flux decrease after the end of the outburst. This unexpected off state of the source lasted for at most 20 days after which SXP 1062 returned to the level observed during previous campaigns. We discuss this and other findings in context of the modern models of accretion onto strongly magnetized neutron stars.
Key words: accretion, accretion disks / X-rays: binaries / stars: magnetic field / stars: neutron / scattering / pulsars: general
© ESO 2020
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