Optical and X-ray outbursts of Be/X-ray binary system SAX J2103.5+4545

Kızıloğlu, Ü.; Ozbilgen, S.; Kiziloglu, N.; Baykal, A.

doi:10.1051/0004-6361/200912638

Cited by 8 publications

(9 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Assuming a 6.5 kpc distance , the luminosity dropped from ∼7 to ∼0.01 × 10 36 erg s −1 . Similar values have previously been observed at high states (Galis et al 2007;Baykal et al 2007;Camero Arranz et al 2007;Kızıloǧlu et al 2009;Reig et al 2010). The quiescent luminosity observed from this source with RXTE/PCA is of the order of our XRT determination.…”

Section: X-ray Behavioursupporting

confidence: 92%

“…Figures 2 and 7 corroborate that the optical outbursts of SAX J2103.5+4545 started about three months before the X-ray activity (see also Kızıloǧlu et al 2009). These episodes may be explained as mass-ejection events from the donor star that will provide the material for the Be disc formation (see e.g.…”

Section: Long-term Be-disc/neutron Star Interactionsupporting

confidence: 71%

“…After three years in a low-luminosity state, the source was detected in 2007 April during INTEGRAL observations of the Galactic plane (Galis et al 2007), anticipating a strong outburst also observed by Swift (Krimm et al 2007;Kızıloǧlu et al 2009). Coinciding with the renewed X-ray activity, the optical counterpart showed an H α line in emission in 2007 May, evidence of disc formation around the Be star (Manousakis et al 2007;Kızıloǧlu et al 2009;Reig et al 2010).…”

Section: Introductionmentioning

confidence: 91%

“…At this moment, although the current behaviour of this source so far resembles the activity displayed in 2012, the intensity in the BV filters is slightly brighter than before. As in Kızıloǧlu et al (2009), we searched for periodicity in the ROTSEIIId light curve, but nothing was observed on shorter time scales. All the available data for this source in this band show that the recurrence of the optical outbursts is highly variable.…”

Section: Optical and Ir Photometrymentioning

confidence: 99%

“…All the available data for this source in this band show that the recurrence of the optical outbursts is highly variable. The time span is ∼5 to ∼3 yr (see also Reig et al 2010;Kızıloǧlu et al 2009), or, more recently, shorter than 2 yr.…”

Section: Optical and Ir Photometrymentioning

confidence: 99%

See 4 more Smart Citations

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Camero

Zurita

Gutiérrez‐Soto

et al. 2014

A&A

View full text Add to dashboard Cite

Aims. We present a multiwavelength study of the Be/X-ray binary system SAX J2103.5+4545 with the goal of better characterizing the transient behaviour of this source. Methods. SAX J2103.5+4545 was observed by Swift/XRT four times in 2007 from April 25 to May 5, and during quiescence in 2012 August 31. In addition, this source has been monitored from the ground-based astronomical observatories of El Teide (Tenerife, Spain), Roque de los Muchachos (La Palma, Spain), and Sierra Nevada (Granada, Spain) since 2011 August, and from the TÜBİTAK National Observatory (Antalya, Turkey) since 2009 June. We performed spectral and photometric temporal analyses to investigate the different states exhibited by SAX J2103.5+4545. Results. In X-rays, an absorbed power-law model provided the best fit for all the XRT spectra. An iron-line feature at ∼6.42 keV was present in all the observations except for that taken during quiescence in 2012. The photon indexes are consistent with previous studies of SAX J2103.5+4545 in high/low-luminosity states. Pulsations were found in all the XRT data from 2007 (2.839(2) mHz; MJD 54 222.02), but not during quiescence. The two optical outbursts in 2010 and 2012 lasted for about eight or nine months (as the one in 2007 probably did and the current one in 2014 might do) and were most probably caused by mass-ejection events from the Be star that eventually fed the circumstellar disc. All of these outbursts started about three months before the triggering of the X-ray activity, and at about the same period before the maximum of the Hα line equivalent width (in emission) was reached at only ∼-5 Å. The global correlation between the BV variability and the X-ray intensity was also observed at longer wavelengths in the IR domain.

show abstract

Section: X-ray Behavioursupporting

confidence: 92%

Section: Long-term Be-disc/neutron Star Interactionsupporting

confidence: 71%

Section: Introductionmentioning

confidence: 91%

Section: Optical and Ir Photometrymentioning

confidence: 99%

Section: Optical and Ir Photometrymentioning

confidence: 99%

See 3 more Smart Citations

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Camero

Zurita

Gutiérrez‐Soto

et al. 2014

A&A

View full text Add to dashboard Cite

show abstract

A pipeline for the ROTSE–IIId archival data

et al. 2012

View full text Add to dashboard Cite

We have constructed a new, fast, robust and reliable pipeline to detect variable stars from the ROTSE-IIId archival data. Turkish share of ROTSE-III archive contains approximately one million objects from a large field of view (1.85 • ) and it considerably covers a large portion of northern sky (δ > −25 • ). The unfiltered ROTSE-III magnitude of the objects ranges from 7.7 to 16.9. The main stages of the new pipeline are as follows: Source extraction, astrometry of the objects, light curve generation and inhomogeneous ensemble photometry. A high performance computing (HPC) algorithm has also been implemented into the pipeline where we had a good performance even on a personal computer. Running the algorithms of the pipeline on a cluster decreases analysis time significantly from weeks to hours. The pipeline is especially tested against long period variable stars with periods of a few hundred days (e.g Mira and SR) and variables having periods starting from a few days to a few hundred days were detected.

show abstract

Finding a 24-day orbital period for the X-ray binary 1A 1118-616

Staubert

Pottschmidt

Doroshenko

et al. 2011

A&A

View full text Add to dashboard Cite

We report the first determination of the binary period and orbital ephemeris of the Be X-ray binary containing the pulsar 1A 1118-616 (35 years after the discovery of the source). The orbital period is found to be P orb = 24.0 ± 0.4 days. The source was observed by RXTE during its last large X-ray outburst in January 2009, which peaked at MJD 54845.4, by taking short observations every few days, covering an elapsed time comparable to the orbital period. Using the phase connection technique, pulse arrival time delays could be measured and an orbital solution determined. The data are consistent with a circular orbit and the time of 90 degrees longitude was found to be T π/2 = MJD 54845.37(10), which is coincident with that of the peak X-ray flux.

show abstract

Optical and X-ray outbursts of Be/X-ray binary system SAX J2103.5+4545

Cited by 8 publications

References 35 publications

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

Recent activity of the Be/X-ray binary system SAX J2103.5+4545

A pipeline for the ROTSE–IIId archival data

Finding a 24-day orbital period for the X-ray binary 1A 1118-616

Contact Info

Product

Resources

About