Long-term evolution of the neutron-star spin period of SXP 1062

Sturm, R.; Haberl, F.; Oskinova, L. M.; Schurch, M. P. E.; Hénault-Brunet, V.; Gallagher, J.; Udalski, A.

doi:10.1051/0004-6361/201321755

Cited by 16 publications

(28 citation statements)

References 32 publications

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“…Gonzales-Galan et al (2017) noted optical variation on the order of ∼ 0.6 mag in archival SALT and OGLE data. The first two optical outbursts suggested P orb 656 ± 2 days (Schmidtke et al 2012), with further confirmation due to the fast rise and exponential decay of these outbursts, as noted by Strum et al (2013). Subsequently Gonzales-Galan et al (2017) refined P orb to 668 ± 10 days.…”

Section: Optical Counterpartmentioning

confidence: 82%

On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062

Cappallo

Laycock

Christodoulou

et al. 2020

Monthly Notices of the Royal Astronomical Society

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SXP 1062 is a long-period X-ray pulsar (XRP) with a Be optical companion located in the Small Magellanic Cloud. First discovered in 2010 from XMM–Newton data, it has been the target of multiple observational campaigns due to the seeming incongruity between its long spin period and recent birth. In our continuing modelling efforts to determine the inclination angle (i) and magnetic axis angle (θ) of XRPs, we have fitted 19 pulse profiles from SXP 1062 with our pulsar model, Polestar, including three consecutive Chandra observations taken during the trailing end of a Type I outburst. These fittings have resulted in most likely values of i = 76○ ± 2○ and θ = 40○ ± 9○. SXP 1062 mostly displays a stable double-peaked pulse profile with the peaks separated by roughly a third of a phase, but recently the pulsar has spun up and widened to a spacing of roughly half of a phase, yet the Polestar fits for i and θ remain constant. Additionally, we note a possible correlation between the X-ray luminosity and the separation of the peaks in the pulse profiles corresponding to the highest luminosity states.

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Section: Optical Counterpartmentioning

confidence: 82%

On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062

Cappallo

Laycock

Christodoulou

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…A 3σ evidence for Fe Kα emission line at 6.4 keV is also reported by Sturm et al (2013). Furthermore, a search for a proton cyclotron absorption line on the 0.2-10 keV continuum yields no significant evidence (Sturm et al 2013).…”

Section: Introductionmentioning

confidence: 78%

“…where t o is the folding epoch, ν o is the spin frequency and ν o is the derivative of the spin frequency, respectively. We expand TOAs around the spin-down rate previously reported by Sturm et al (2013) and obtain a phase coherent timing solution (see the upper panel of Fig. 2). We find that the source is spinning down with a rate of ν o = − 4.29(7) × 10 −14 Hz s −1 between MJD 56209 and MJD 56830 (see Table 1).…”

Section: Timing Analysismentioning

confidence: 99%

“…First four pulse period measurements of SXP 1062 in 2010, demonstrate a very high spin-down rate of ν = − 2.6 × 10 −12 Hz s −1 during a short observation interval of 18 days (Haberl et al 2012). The following period is measured ∼ 2.5 years later, which implies a 40 factor lower long term spin-down rate (Sturm et al 2013). In view of the fact that most BeXRBs show spin-up during their outbursts (Bildsten et al 1997), SXP 1062 is atypical with its strong spin-down.…”

Section: Introductionmentioning

confidence: 97%

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Discovery of a glitch in the accretion-powered pulsar SXP 1062

Serim

Şahiner

Cerri-Serim

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present timing analysis of the accretion powered pulsar SXP 1062, based on the observations of Swift, XMM-Newton and Chandra satellites covering a time span of about 2 years. We obtain a phase coherent timing solution which shows that SXP 1062 has been steadily spinning down with a rate − 4.29(7) × 10 −14 Hz s −1 leading to a surface magnetic field estimate of about 1.5 × 10 14 G. We also resolve the binary orbital motion of the system from X-ray data which confirms an orbital period of 656(2) days. On MJD 56834.5, a sudden change in pulse frequency occurs with ∆ν = 1.28(5) × 10 −6 Hz, which indicates a glitch event. The fractional size of the glitch is ∆ν/ν ∼ 1.37(6) ×10 −3 and SXP 1062 continues to spin-down with a steady rate after the glitch. A short X-ray outburst 25 days prior to the glitch does not alter the spin-down of the source; therefore the glitch should be associated with the internal structure of the neutron star. While glitch events are common for isolated pulsars, the glitch of SXP 1062 is the first confirmation of the observability of this type of events among accretion powered pulsars. Furthermore, the value of the fractional change of pulse frequency ensures that we discover the largest glitch reported up to now.

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“…This provides an estimate for the age of the NS in this system, ∼ (2-4)×10 4 yr (Haberl et al 2012;Hénault-Brunet et al 2012). If we assume that the source is close to spin equilibrium (new observations support it, Sturm et al 2013), then the present day field is ∼ 10 13 G. With such short age it is difficult to come to the stage of accretion and spin-down the NS to a 1062 s period. There are two possibilities.…”

Section: High-mass X-ray Binaries and Ns Evolutionmentioning

confidence: 99%

Unifying neutron stars getting to GUNS

2014

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The variety of the observational appearance of young isolated neutron stars must find an explanation in the framework of some unifying approach. Nowadays it is believed that such scenario must include magnetic field decay, the possibility of magnetic field emergence on a time scale of 10 4 -10 5 yr, significant contribution of non-dipolar fields, and appropriate initial parameter distributions. We present our results on the initial spin period distribution, and suggest that inconsistencies between distributions derived by different methods for samples with different average ages can uncover field decay or/and emerging field. We describe a new method to probe the magnetic field decay in normal pulsars. The method is a modified pulsar current approach, where we study pulsar flow along the line of increasing characteristic age for constant field. Our calculations, performed with this method, can be fitted with an exponential decay for ages in the range of 8×10 4 -3.5×105 yr with a time scale of ∼ 5×10 5 yr. We discuss several issues related to the unifying scenario. At first, we note that the dichotomy, among local thermally emitting neutron stars, between normal pulsars and the Magnificent Seven remains unexplained. Then we discuss the role of high-mass X-ray binaries in the unification of neutron star evolution. We note, that such systems allow to check evolutionary effects on a time scale longer than what can be probed with normal pulsars alone. We conclude with a brief discussion of the importance of discovering old neutron stars accreting from the interstellar medium.

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Long-term evolution of the neutron-star spin period of SXP 1062

Cited by 16 publications

References 32 publications

On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062

On the Geometry of the X-ray emission from pulsars a consistent inclination and beaming solution for the Be/X-ray pulsar SXP 1062

Discovery of a glitch in the accretion-powered pulsar SXP 1062

Unifying neutron stars getting to GUNS

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