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

Islam, Nazma; Paul, Biswajit

doi:10.1093/mnras/stw1299

Cited by 19 publications

(11 citation statements)

References 54 publications

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“…The BAT all sky monitor (ASM) lightcurve between 57000-58500 MJD has been barycenter corrected using the earth2sun package available in HEASOFT. Using the ftool efsearch on it, the orbital period is found to be 294764.55 ± 68.78 s (∼3.411627 days), which is consistent with the result published earlier (Islam & Paul 2016). For NuSTAR and XRT data barycorr has been used to apply the barycentric correction and for LAXPC data the standard ASTROSAT tool as1bary has been used for the same.…”

Section: Timing Analysissupporting

confidence: 85%

“…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%

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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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Section: Timing Analysissupporting

confidence: 85%

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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“…(1) Islam & Paul (2016); (2) Notes. (a) uncertain mounted at the 2.2 m telescope operated at the European Southern Observatory (ESO) in La Silla.…”

Section: Igr J11305-6256mentioning

confidence: 99%

The stellar and wind parameters of six prototypical HMXBs and their evolutionary status

Hainich

Oskinova

Torrejón

et al. 2020

A&A

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Context. High-mass X-ray binaries (HMXBs) are exceptional astrophysical laboratories that offer a rare glimpse into the physical processes that govern accretion on compact objects, massive-star winds, and stellar evolution. In a subset of the HMXBs, the compact objects accrete matter solely from winds of massive donor stars. These so-called wind-fed HMXBs are divided in persistent (classical) HMXBs and supergiant fast X-ray transients (SFXTs) according to their X-ray properties. While it has been suggested that this dichotomy depends on the characteristics of stellar winds, they have been poorly studied. Aims. With this investigation, we aim to remedy this situation by systematically analyzing donor stars of wind-fed HMXBs that are observable in the UV, concentrating on those with neutron star (NS) companions. Methods. We obtained Swift X-ray data, HST UV spectra, and additional optical spectra for all our targets. The spectral analysis of our program stars was carried out with the Potsdam Wolf-Rayet (PoWR) model atmosphere code. Results. Our multi-wavelength approach allows us to provide stellar and wind parameters for six donor stars (four wind-fed systems and two OBe X-ray binaries). The wind properties are in line with the predictions of the line-driven wind theory. Based on the abundances, three of the donor stars are in an advanced evolutionary stage, while for some of the stars, the abundance pattern indicates that processed material might have been accreted. When passing by the NS in its tight orbit, the donor star wind has not yet reached its terminal velocity but it is still significantly slower; its speed is comparable with the orbital velocity of the NS companion. There are no systematic differences between the two types of wind-fed HMXBs (persistent versus transients) with respect to the donor stars. For the SFXTs in our sample, the orbital eccentricity is decisive for their transient X-ray nature. The dichotomy of wind-fed HMXBs studied in this work is primarily a result of the orbital configuration, while in general it is likely that it reflects a complex interplay between the donor-star parameters, the orbital configuration, and the NS properties. Based on the orbital parameters and the further evolution of the donor stars, the investigated HMXBs will presumably form Thorne-Żytkow objects in the future.

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“…Apsidal advance has also been detected in the transient X-ray binary 4U 0115+63 using pulse timing (Raichur and Paul 2010b). In the absence of pulsations, eclipse measurements have been used in 4U 1700-37 (Islam and Paul 2016), the rate of evolution of which was earlier overestimated as the effect of intrinsic rapid intensity variation of the source during the eclipse transitions was not taken into account. With the exception of Cyg X-3, the orbital periods of the HMXBs are found to decay.…”

Section: Evolution Of High Mass X-ray Binariesmentioning

confidence: 99%

Neutron Stars in X-ray Binaries and their Environments

Paul

2017

J Astrophys Astron

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Abstract.Neutron stars in X-ray binary systems are fascinating objects that display a wide range of timing and spectral phenomena in the X-rays. Not only parameters of the neutron stars, like magnetic field strength and spin period evolve in their active binary phase, the neutron stars also affect the binary systems and their immediate surroundings in many ways. Here we discuss some aspects of the interactions of the neutron stars with their environments that are revelaed from their X-ray emission. We discuss some recent developments involving the process of accretion onto high magnetic field neutron stars: accretion stream structure and formation, shape of pulse profile and its changes with accretion torque. Various recent studies of reprocessing of X-rays in the accretion disk surface, vertical structures of the accretion disk and wind of companion star are also discussed here. The X-ray pulsars among the binary neutron stars provide excellent handle to make accurate measurement of the orbital parameters and thus also evolution of the binray orbits that take place over time scale of a fraction of a million years to tens of millions of years. The orbital period evolution of X-ray binaries have shown them to be rather complex systems. Orbital evolution of X-ray binaries can also be carried out from timing of the X-ray eclipses and there have been some surprising results in that direction, including orbital period glitches in two X-ray binaries and possible detection of the most massive circum-binary planet around a Low Mass X-ray Binary.

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

Cited by 19 publications

References 54 publications

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

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

The stellar and wind parameters of six prototypical HMXBs and their evolutionary status

Neutron Stars in X-ray Binaries and their Environments

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