<i>RXTE</i>
                    Discovery of Multiple Cyclotron Lines during the 2004 December Outburst of V0332+53

Pottschmidt, K.; Kreykenbohm, I.; Wilms, J.; Coburn, W.; Rothschild, R. E.; Kretschmar, P.; McBride, V. A.; Suchy, S.; Staubert, R.

doi:10.1086/498689

Cited by 82 publications

(117 citation statements)

References 22 publications

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“…However, there is a qualitative agreement of the Suzaku data and the results by Fürst et al (2014) regarding the CRSF. Although observed in a number of other sources (e.g., 4U 0115+634 or V 0332+53, Heindl et al 1999;Pottschmidt et al 2005, respectively), we find no indications of a second harmonic, which we would expect around 24 keV, although PIN and NuSTAR are both very sensitive in this energy The best-fit parameters are given in Table 2, and Fig. 5 shows the phase-averaged spectrum and best-fit model of the second observation.…”

Section: Phase-averaged Spectroscopycontrasting

confidence: 48%

Suzakuobservations of the 2013 outburst of KS 1947+300

Ballhausen

Kühnel

Pottschmidt

et al. 2016

A&A

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We report on the timing and spectral analysis of two Suzaku observations with different flux levels of the high-mass X-ray binary KS 1947+300 during its 2013 outburst. In agreement with simultaneous NuSTAR observations, the continuum is well described by an absorbed power law with a cutoff and an additional blackbody component. In addition, we find fluorescent emission from neutral, Helike, and even H-like iron. We determine a pulse period of ∼18.8 s with the source showing a spin-up between the two observations. Both Suzaku observations show very similar behavior of the pulse profile, which is strongly energy dependent. This profile has an evolution from a profile with one peak at low energies to a profile with two peaks of different widths toward higher energies seen in both the Suzaku and NuSTAR data. Such an evolution to a more complex profile at higher energies is rarely seen in X-ray pulsars, most cases show the opposite behavior. Pulse phase-resolved spectral analysis shows a variation in the absorbing column density, N H , over pulse phase. Spectra taken during the pulse profile minima are intrinsically softer compared to the pulse phase-averaged spectrum.

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Section: Phase-averaged Spectroscopycontrasting

confidence: 48%

Suzakuobservations of the 2013 outburst of KS 1947+300

Ballhausen

Kühnel

Pottschmidt

et al. 2016

A&A

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“…The next powerful outburst of V 0332+53 began at the end of 2004 ). An analysis of the follow-up observations performed with the RXTE and INTEGRAL observatories showed that beside the absorption feature at an energy of ∼ 26 keV, there are two additional similar features in the source spectrum at energies of ∼ 49 and ∼ 75 keV, which were interpreted as the second and third harmonics of the main cyclotron frequency Pottschmidt et al, 2005). A good coverage of the whole outburst (including rising and declining parts) with the RXTE observations allowed to Tsygankov et al (2006Tsygankov et al ( , 2010 to make a detailed spectral analysis and to show that the cyclotron line energy is not a constant but negatively correlated with the source luminosity and to obtain constraints on the magnetic field in the source as B NS ≃ 3.5 × 10 12 G. Moreover, the line energy as well as its width and depth are also strongly variable on the pulse period scale .…”

Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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“…1 that the model adequately describes observations in a wide energy range 3-100 keV. Pottschmidt et al (2005) and Nakajima et al (2010) have discussed a complex structure of the V 0332+53 spectrum near the cyclotron line. This is also visible in the residuals of our spectra.…”

Section: Observations Spectral Model and Data Analysismentioning

confidence: 92%

Transient X-ray pulsar V 0332+53: pulse-phase-resolved spectroscopy and the reflection model

Lutovinov¹,

Tsygankov²,

Suleimanov³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present the results of the pulse phase-and luminosity-resolved spectroscopy of the transient X-ray pulsar V 0332+53, performed for the first time in a wide luminosity range (1 − 40) × 10 37 erg s −1 during a giant outburst observed by the RXTE observatory in Dec 2004 -Feb 2005. We characterize the spectra quantitatively and built the detailed "threedimensional" picture of spectral variations with pulse phase and throughout the outburst. We show that all spectral parameters are strongly variable with the pulse phase, and the pattern of this variability significantly changes with luminosity directly reflecting the associated changes in the structure of emission regions and their beam patterns. Obtained results are qualitatively discussed in terms of the recently developed reflection model for the formation of cyclotron lines in the spectra of X-ray pulsars.

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RXTE Discovery of Multiple Cyclotron Lines during the 2004 December Outburst of V0332+53

Cited by 82 publications

References 22 publications

Suzakuobservations of the 2013 outburst of KS 1947+300

Suzakuobservations of the 2013 outburst of KS 1947+300

High-mass X-ray binaries in the Milky Way

Transient X-ray pulsar V 0332+53: pulse-phase-resolved spectroscopy and the reflection model

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