@article{SturmHaberlOskinovaetal.2013,
  author    = {Sturm, R. and Haberl, F. and Oskinova, Lida and Schurch, M. P. E. and Henault-Brunet, V. and Gallagher, J. S. and Udalski, A.},
  title     = {Long-term evolution of the neutron-star spin period of SXP1062},
  series = {Astronomy and astrophysics : an international weekly journal},
  volume    = {556},
  journal   = {Astronomy and astrophysics : an international weekly journal},
  number    = {4},
  publisher = {EDP Sciences},
  address   = {Les Ulis},
  issn      = {0004-6361},
  doi       = {10.1051/0004-6361/201321755},
  pages     = {8},
  year      = {2013},
  abstract  = {Context. The Be/X-ray binary SXP 1062 is of especial interest owing to the large spin period of the neutron star, its large spin-down rate, and the association with a supernova remnant constraining its age. This makes the source an important probe for accretion physics. Aims. To investigate the long-term evolution of the spin period and associated spectral variations, we performed an XMM-Newton target-of-opportunity observation of SXP 1062 during X-ray outburst. Methods. Spectral and timing analysis of the XMM-Newton data was compared with previous studies, as well as complementary Swift/XRT monitoring and optical spectroscopy with the SALT telescope were obtained. Results. The spin period was measured to be P-s = (1071.01 +/- 0.16) s on 2012 Oct. 14. The X-ray spectrum is similar to that of previous observations. No convincing cyclotron absorption features, which could be indicative for a high magnetic field strength, are found. The high-resolution RGS spectra indicate the presence of emission lines, which may not completely be accounted for by the SNR emission. The comparison of multi-epoch optical spectra suggest an increasing size or density of the decretion disc around the Be star. Conclusions. SXP 1062 showed a net spin-down with an average of P-s = ( 2.27 +/- 0.44) s yr(-1) over a baseline of 915 days.},
  language  = {en}
}