The radial velocity curve of HD 153919 (4U 1700-37) revisited

Hammerschlag-Hensberge, G.; Kerkwijk, M. H. van; Kaper, L.

doi:10.1051/0004-6361:20030962

Cited by 15 publications

(29 citation statements)

References 19 publications

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“…IGR J17252-3616) Zurita Heras et al (2006), Thompson et al (2007), Manousakis & Walter (2011); (i) Baykal et al (2011. ( j) The eccentricity for this source has been reported by Hammerschlag-Hensberge et al (2003) to be 0.22(4), which was later challenged by Clark (2000) and this work. (k) Mid-eclipse time, equivalent to the time when the mean longitude l equals π/2 for a circular orbit.…”

Section: Introductionmentioning

confidence: 66%

“…(a) Levine et al (2000), Bildsten et al (1997) but see also Naik & Paul (2004); (b) Bildsten et al (1997), Raichur & Paul (2010b); (c) Rubin et al (1996), Hammerschlag-Hensberge et al (2003); (d) Mukherjee et al (2006), Clark (2000); (e) Inam et al (2010), Raichur & Paul (2010b); ( f ) (a.k.a. IGR J18027-2016) Hill et al (2005); (g) Corbet & Mukai (2002); (h) (a.k.a.…”

Section: Introductionmentioning

confidence: 99%

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Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Falanga

Bozzo

Lutovinov

et al. 2015

A&A

188

265

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We update the ephemeris of the eclipsing high-mass X-ray binary (HMXB) systems LMC X-4, Cen X-3, 4U 1700-377, 4U 1538-522, SMC X-1, IGR J18027-2016, Vela X-1,IGR J17252-3616, XTE J1855-026, and OAO 1657-415 with the help of more than ten years of monitoring these sources with the All Sky Monitor onboard RXTE and with the Integral Soft Gamma-Ray Imager onboard INTEGRAL. These results are used to refine previous measurements of the orbital period decay of all sources (where available) and provide the first accurate values of the apsidal advance in Vela X-1 and 4U 1538-522. Updated values for the masses of the neutron stars hosted in the ten HMXBs are also provided, as well as the long-term light curves folded on the best determined orbital parameters of the sources. These light curves reveal complex eclipse ingresses and egresses that are understood mostly as being caused by accretion wakes. Our results constitute a database to be used for population and evolutionary studies of HMXBs and for theoretical modeling of long-term accretion in wind-fed X-ray binaries.

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Section: Introductionmentioning

confidence: 66%

Section: Introductionmentioning

confidence: 99%

Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Falanga

Bozzo

Lutovinov

et al. 2015

A&A

188

265

View full text Add to dashboard Cite

show abstract

“…The upper limit on eccentricity of the orbit of 4U 1700-37 put from the limits of residuals in the mid-eclipse times and limits on variation in the eclipse duration is quite low; e ∼ 0.008 and 0.05 respectively. This is in contrast with e ∼ 0.22 from the radial velocity measurements with IUE data (Hammerschlag-Hensberge, van Kerkwijk & Kaper 2003). In the presence of a significant apsidal motion, the radial velocity measurements at different orbital phases (with respect to the mid-eclipse times) in data spread over several years can not be put together in a simple way.…”

Section: Eccentricity Of the Binary Orbitmentioning

confidence: 82%

Orbital evolution and search for eccentricity and apsidal motion in the eclipsing HMXB 4U 1700−37

Islam

Paul

2016

Mon. Not. R. Astron. Soc.

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In the absence of detectable pulsations in the eclipsing High Mass X-ray binary 4U 1700-37, the orbital period decay is necessarily determined from the eclipse timing measurements. We have used the earlier reported mid-eclipse time measurements of 4U 1700-37 together with the new measurements from long term light curves obtained with the all sky monitors RXTE-ASM, Swift-BAT and MAXI-GSC, as well as observations with RXTE-PCA, to measure the long term orbital evolution of the binary. The orbital period decay rate of the system is estimated to bė P /P = −(4.7 ± 1.9) × 10 −7 yr −1 , smaller compared to its previous estimates. We have also used the mid-eclipse times and the eclipse duration measurements obtained from 10 years long X-ray light-curve with Swift-BAT to separately put constraints on the eccentricity of the binary system and attempted to measure any apsidal motion. For an apsidal motion rate greater than 5 degrees per year, the eccentricity is found to be less than 0.008, which limits our ability to determine the apsidal motion rate from the current data. We discuss the discrepancy of the current limit of eccentricity with the earlier reported values from radial velocity measurements of the companion star.

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“…This High Mass X-ray Binary (HMXB) has an orbital period of 3.41 days. The extreme 07 f star HD 153919 is a confirmed optical counterpart (Penny et al 1973;Hutchings et al 1973;Dolan et al 1980), of which an orbital eccentricity of 0.22±0.04 and a radial velocity semi-amplitude of 20.6±1.0 km s −1 have been measured (Hammerschlag-Hensberge et al 2003). The binary parameters of the 4U 1700-37 System are tabulated in Seifina et al (2016) and Islam & Paul (2016).…”

Section: Introductionmentioning

confidence: 99%

Possible detection of a new cyclotron feature in 4U 1700–37

Bala

Roy

Bhattacharya

2020

Monthly Notices of the Royal Astronomical Society

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We present a spectral and timing study of the High Mass X-ray Binary transient source 4U 1700-37 using NuSTAR and ASTROSAT/LAXPC. The source is observed in two different flux states. A combined spectral analysis of NuSTAR's FPMA and FPMB shows the possible hint of a cyclotron line feature at ∼16 keV. The line feature is consistently present in different continuum models with at least 3σ confidence level. We do not detect the presence of a previously reported 39 keV cyclotron line in the combined spectra. A ∼16 keV cyclotron feature would suggest that the compact object is a neutron star with a magnetic field strength ∼ 2.1×10 12 Gauss in the emission region. We also find the presence of a rare Ni Kα emission line around 7.6 keV in the NuSTAR spectrum. We searched the NuSTAR and ASTROSAT data for coherent or quasi-periodic oscillation signals but found no evidence in the frequency range 0.1 mHz to 10 3 Hz.

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The radial velocity curve of HD 153919 (4U 1700-37) revisited

Cited by 15 publications

References 19 publications

Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Ephemeris, orbital decay, and masses of ten eclipsing high-mass X-ray binaries

Orbital evolution and search for eccentricity and apsidal motion in the eclipsing HMXB 4U 1700−37

Possible detection of a new cyclotron feature in 4U 1700–37

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