The Orbital Period of Swift J1626.6–5156

Baykal, A.; Göǧüş, E.; İnam, S. Ç.; Belloni, T.

doi:10.1088/0004-637x/711/2/1306

Cited by 15 publications

(21 citation statements)

References 21 publications

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“…(2007); 16 Staubert et al. (2011); 17 Raichur & Paul (2010b); 18 in’t Zand, Corbet & Marshall (2001); 19 Kelley, Rappaport & Ayasli (1983); 20 Baykal et al. (2010); 21 Scott et al.…”

Section: Discussionmentioning

confidence: 99%

“…If the parameter is known to better than 3 decimal places, it is truncated and the error is smaller than 0.001. References for quantities presented in the Table are given here for each individual system: 1 Kaspi et al (1994); 2 Harmanec et al (2000); 3 Barsukova et al (2005); 10 Finger, Wilson & Hagedon (1994); 11 Hutchings et al (1985); 12 Kaaret, Cusumano & Sacco (2000); 13 Wilson et al (1997); 14 Wang, Johnston & Manchester (2004); 15 Coe et al (2007); 16 Staubert et al (2011); 17 Raichur & Paul (2010b); 18 in't Zand, Corbet & Marshall (2001); 19 Kelley, Rappaport & Ayasli (1983); 20 Baykal et al (2010); 21 Scott et al (1997), Shaw et al (2009);22 Finger et al (1999); 23 Galloway, Wang & Morgan (2005); 24 Wilson et al (2003); 25 Galloway, Morgan & Levine (2004); 26 Wilson, Finger & Camero-Arranz (2008); 27 Baykal et al (2007); 28 Raichur & Paul (2010a); 29 Grundstrom et al (2007); 30 Levine (1991), van der Meer et al (2007); 31 Kreykenbohm et al (2008);…”

Section: Comparison With the Galactic Populationmentioning

confidence: 99%

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On the orbital parameters of Be/X-ray binaries in the Small Magellanic Cloud

Townsend¹,

Coe²,

Corbet³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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The orbital motion of a neutron star about its optical companion presents a window through which we can study the orbital parameters of that binary system. This has been used extensively in the Milky Way to calculate these parameters for several high‐mass X‐ray binaries. Using several years of Rossi X‐ray Timing Explorer Proportional Counter Array data, we derive the orbital parameters of four Be/X‐ray binary systems in the Small Magellanic Cloud (SMC), increasing the number of systems with orbital solutions by a factor of 3. We find one new orbital period, confirm a second and discuss the parameters with comparison to the Galactic systems. Despite the low metallicity in the SMC, these binary systems sit amongst the Galactic distribution of orbital periods and eccentricities, suggesting that metallicity may not play an important role in the evolution of high‐mass X‐ray binary systems. A plot of orbital period against eccentricity shows that the supergiant, Be and low‐eccentricity OB transient systems occupy separate regions of the parameter space; akin to the separated regions on the Corbet diagram. Using a Spearman’s rank correlation test, we also find a possible correlation between the two parameters. The mass functions, inclinations and orbital semimajor axes are derived for the SMC systems based on the binary parameters and the spectral classification of the optical counterpart. As a by‐product of our work, we present a catalogue of the orbital parameters for every high‐mass X‐ray binary in the Galaxy and Magellanic Clouds for which they are known.

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“…(2007); 16 Staubert et al. (2011); 17 Raichur & Paul (2010b); 18 in’t Zand, Corbet & Marshall (2001); 19 Kelley, Rappaport & Ayasli (1983); 20 Baykal et al. (2010); 21 Scott et al.…”

Section: Discussionmentioning

confidence: 99%

Section: Comparison With the Galactic Populationmentioning

confidence: 99%

On the orbital parameters of Be/X-ray binaries in the Small Magellanic Cloud

Townsend¹,

Coe²,

Corbet³

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…The fluctuation on the residuals is consistent with Doppler delays due to orbital motion. In general for an eccentric orbit, it can be represented as (Deeter et al 1981)(see also in't Zand et al 2001;Baykal et al 2000Baykal et al , 2010, for applications)…”

Section: Timing Analysismentioning

confidence: 99%

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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“…A Lomb-Scargle periodogram (Lomb 1976;Scargle 1982) of the light curve first revealed an oscillation period from ∼JD 2454000-JD 2454350 September-2007 of ∼47 days and from ∼JD 2454350-2454790 (2007September-2008 of ∼3/2 of this, or ∼72.5 days (DeCesar et al 2009). Recent work by Baykal et al 2010 found the long-term variability timescale to range from ∼45 to 95 days. Additionally, from pulse timing analysis, they find the binary orbit to be nearly circular (eccentricity 0.08) with a period of 132.9 days, meaning the oscillations occur on timescales of ∼1/2 and ∼2/3 of the orbital period.…”

Section: Introductionmentioning

confidence: 99%

THE Be/X-RAY BINARY SWIFT J1626.6–5156 AS A VARIABLE CYCLOTRON LINE SOURCE

DeCesar

Boyd

Pottschmidt

et al. 2012

ApJ

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Swift J1626.6−5156 is a Be/X-ray binary that was in outburst from December 2005 until November 2008. We have examined RXTE/PCA and HEXTE spectra of three long observations of this source taken early in its outburst, when the PCA 2-20 keV count rate was >70 counts s −1 PCU −1 , as well as several combined observations from different stages of the outburst. The spectra are best fit with an absorbed cutoff power law with a ∼ 6.4 keV iron emission line and a Gaussian optical depth absorption line at ∼10 keV. We present strong evidence that this absorption-like feature is a cyclotron resonance scattering feature, making Swift J1626.6−5156 a new candidate cyclotron line source. The redshifted energy of ∼10 keV implies a magnetic field strength of ∼ 8.6(1 + z) × 10 11 G in the region of the accretion column close to the magnetic poles where the cyclotron line is produced. Analysis of phase averaged spectra spanning the duration of the outburst suggests a possible positive correlation between the fundamental cyclotron energy and source luminosity. Phase resolved spectroscopy from a long observation reveals a variable cyclotron line energy, with phase dependence similar to a variety of other pulsars, as well as the first harmonic of the fundamental cyclotron line.

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The Orbital Period of Swift J1626.6–5156

Cited by 15 publications

References 21 publications

On the orbital parameters of Be/X-ray binaries in the Small Magellanic Cloud

On the orbital parameters of Be/X-ray binaries in the Small Magellanic Cloud

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

THE Be/X-RAY BINARY SWIFT J1626.6–5156 AS A VARIABLE CYCLOTRON LINE SOURCE

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