Long-term evolution of the neutron-star spin period of SXP1062

被引:11
作者
Sturm, R. [1 ]
Haberl, F. [1 ]
Oskinova, L. M. [2 ]
Schurch, M. P. E. [3 ]
Henault-Brunet, V. [4 ]
Gallagher, J. S., III [5 ]
Udalski, A. [6 ]
机构
[1] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany
[2] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany
[3] Univ Cape Town, Dept Astron, Astrophys Cosmol & Grav Ctr ACGC, ZA-7701 Rondebosch, South Africa
[4] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland
[5] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA
[6] Univ Warsaw Observ, PL-00478 Warsaw, Poland
来源
ASTRONOMY & ASTROPHYSICS | 2013年 / 556卷
基金
欧洲研究理事会; 新加坡国家研究基金会;
关键词
pulsars: individual: SXP1062; galaxies: individual: Small Magellanic Cloud; stars:; emission-line; Be; stars: neutron; X-rays: binaries; SMALL-MAGELLANIC-CLOUD; AFRICAN LARGE TELESCOPE; FOCUS IMAGING SPECTROGRAPH; X-RAY PULSARS; XMM-NEWTON; SXP; 1062; LIKELIHOOD RATIO; BINARY; YOUNG; DISCOVERY;
D O I
10.1051/0004-6361/201321755
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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.
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页数:8
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