The slow X-ray pulsar SXP1062 and associated supernova remnant in the Wing of the Small Magellanic Cloud

L.M. Oskinova1, M.A. Guerrero2, V. Henault-Brunet3, W. Sun4, Y.-H. Chu5, C.J. Evans3, J.S. Gallagher III6, R.A. Gruendl5, J. Reyes-Iturbide7

1 Institute for Physics and Astronomy, University of Potsdam, Germany
2 Instituto de Astrofisica de Andalucia, Granada, Spain
3 Institute for Astronomy, University of Edinburgh, UK
4 Department of Astronomy, Nanjing University, China
5 Department of Astronomy, University of Illinois, USA
6 Department of Astronomy, University of Wisconsin-Madison, USA
7 Escuela Superior de Fisica y Matematicas, Mexico

SXP1062 is an exceptional case of a young neutron star in a wind-fed high-mass X-ray binary associated with a supernova remnant. A unique combination of measured spin period, its derivative, luminosity and young age makes this source a key probe for the physics of accretion and neutron star evolution. Theoretical models proposed to explain the properties of SXP1062 shall be tested with new data.

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