<i>Chandra</i>Grating Spectroscopy of the X‐Ray Binary 4U 1700−37 in a Flaring State

Boroson, Bram; Vrtilek, S. D.; Kallman, T. R.; Corcoran, M. F.

doi:10.1086/375636

Cited by 54 publications

(83 citation statements)

References 49 publications

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“…The presence of dense matter in this orbital phase range can be the possible reason for the eclipse like segments. Such type of eclipse-like segments (quiescence period) was also observed during Chandra observation of 4U 1700-37 around ∼0.68 orbital phase (Boroson et al 2003). A significant increase in the column density after phase 0.5 was also reported earlier during the Copernicus observation of 4U 1700-37 (Mason et al 1976).…”

Section: Discussionsupporting

confidence: 80%

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Broad-band spectroscopy of the eclipsing high-mass X-ray binary 4U 1700-37 with Suzaku

Jaisawal

Naik

2015

Monthly Notices of the Royal Astronomical Society

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We present the results obtained from broadband spectroscopy of the high mass X-ray binary 4U 1700-37 using data from a Suzaku observation in 2006 September 13-14 covering 0.29-0.72 orbital phase range. The light curves showed significant and rapid variation in source flux during entire observation. We did not find any signature of pulsations in the light curves. However, a quasi-periodic oscillation at ∼20 mHz was detected in the power density spectrum of the source. The 1-70 keV spectrum was fitted with various continuum models. However, we found that the partially absorbed high energy cutoff power-law and Negative and Positive power-law with Exponential cutoff (NPEX) models described the source spectrum well. Iron emission lines at 6.4 keV and 7.1 keV were detected in the source spectrum. An absorption like feature at ∼39 keV was detected in the residuals while fitting the data with NPEX model. Considering the feature as cyclotron absorption line, the surface magnetic field of the neutron star was estimated to be ∼3.4×1012 Gauss. To understand the cause of rapid variation in the source flux, time-resolved spectroscopy was carried out by dividing the observation into 20 narrow segments. The results obtained from the time-resolved spectroscopy are interpreted as the accretion of inhomogeneously distributed matter in the stellar wind of the supergiant companion star as the cause of observed flux variation in 4U 1700-37. A sharp increase in column density after ∼0.63 orbital phase indicates the presence of an accretion wake that blocks the continuum and produces the eclipse like low-flux segment.

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Section: Discussionsupporting

confidence: 80%

“…Presence of recombination lines from H and He atoms in eclipse phase suggested an extended ionization region around the source. As in the case of accretion powered X-ray pulsars, several mHz QPOs were also detected in the power density spectra of 4U 1700-37, obtained from the Chadra observation (Boroson et al 2003).…”

Section: Introductionmentioning

confidence: 58%

Broad-band spectroscopy of the eclipsing high-mass X-ray binary 4U 1700-37 with Suzaku

Jaisawal

Naik

2015

Monthly Notices of the Royal Astronomical Society

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“…The binary may have escaped the Sco OB1 association 2 millions years ago (Ankay et al, 2001). High-ionisation lines have been observed also during eclipses, indicating that the stellar wind is very inhomogeneous (Boroson et al, 2003). The hard X-ray flux varies by a factor of several hundreds.…”

Section: Discussionmentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

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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“…Other X-ray continuum models of high-mass X-ray binaries (HMXBs), such as two absorbed power laws or three absorbed power laws, can also describe the observations with ASCA of Vela X−1 (Sako et al 1999) or with Chandra & XMM-Newton of 4U 1700−37 (Boroson et al 2003;van der Meer et al 2005). One power law is used to fit the direct continuum, which originates near the neutron star.…”

Section: Spectral Analysismentioning

confidence: 99%

“…We obtained a good description of the spectrum (χ 2 ν = 1.20, F-test of 11 × 10 −116 ), but a significantly worse fit than the previous components (χ 2 ν = 1.16). Finally, we modelled the soft X-ray continuum component with only a blend of Gaussians (Boroson et al 2003;van der Meer et al 2005) and refitted the data. We could not obtain a good description below 0.6 keV, though.…”

Section: X-ray Continuummentioning

confidence: 99%

Detecting emission lines withXMM-Newtonin 4U 1538–52

Roca

Page

Torrejón

et al. 2010

A&A

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Context. The properties of the X-ray emission lines are a fundamental tool for studying the nature of the matter surrounding the neutron star and the phenomena that produce these lines. Aims. The aim of this work is to analyse the X-ray spectrum of 4U 1538−52 obtained by the XMM-Newton observatory and to look for the presence of diagnostic lines in the energy range 0.3−11.5 keV. Methods. We used a 54 ks PN & MOS/XMM-Newton observation of the high-mass X-ray binary 4U 1538−52 covering the orbital phase between 0.75 to 1.00 (the eclipse ingress). We modelled the 0.3−11.5 keV continuum emission with three absorbed power laws and looked for the emission lines. Results. We found previously unreported recombination lines in this system at ∼2.4 keV, ∼1.9 keV, and ∼1.3 keV, which is consistent with the presence of highly ionized states of S XV Heα, Si XIII Heα, and either Mg Kα or Mg XI Heα. On the other hand, in spectra that are both out of eclipse and in eclipse, we detect a fluorescence iron emission line at 6.4 keV, which is resolved into two components: a narrow (σ ≤ 10 eV) fluorescence Fe Kα line plus one hot line from highly photoionized Fe XXV. Conclusions. The detection of new recombination lines during eclipse ingress in 4U 1538−52 indicates that there is an extended ionized region surrounding the neutron star.

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ChandraGrating Spectroscopy of the X‐Ray Binary 4U 1700−37 in a Flaring State

Cited by 54 publications

References 49 publications

Broad-band spectroscopy of the eclipsing high-mass X-ray binary 4U 1700-37 with Suzaku

Broad-band spectroscopy of the eclipsing high-mass X-ray binary 4U 1700-37 with Suzaku

High-mass X-ray binaries in the Milky Way

Detecting emission lines withXMM-Newtonin 4U 1538–52

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