A Precise Measurement of the Orbital Period Parameters of Cygnus X-3

Bhargava, Yash; Rao, A. R.; Singh, K. P.; Choudhury, Manojendu; Bhattacharyya, Sudip; Chandra, Sunil; Dewangan, G. C.; Mukerjee, K.; Stewart, G. C.; Bhattacharya, Dipankar; Mithun, N. P. S.; Vadawale, S.

doi:10.3847/1538-4357/aa8ea4

Cited by 15 publications

(16 citation statements)

References 27 publications

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“…They could be improved with future studies of the photometry of the source in quiescence. Also, strong distance constraints could have been achieved if the 5Ṗ has also been measured in the short period (P ≈ 0.20 d) high-mass Xray binary Cyg X-3, whereṖ > 0 and P/Ṗ ≈ 1.0 × 10 6 yr (e.g., Bhargava et al 2017), which value appears to be in agreement with the rate of wind mass loss in that system. However, while it is likely that the compact object in that system is a BH, the presence of a neutron star remains possible (Zdziarski, spectroscopic observations of H17 were accompanied by sensitive photometry.…”

Section: Discussionmentioning

confidence: 78%

The X-ray binary GX 339–4/V821 Ara: the distance, inclination, evolutionary status, and mass transfer

Zdziarski

Ziółkowski

Mikołajewska

2019

Monthly Notices of the Royal Astronomical Society

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We consider constraints on the distance, inclination and component masses in the X-ray binary GX 339-4 resulting from published works, and then construct detailed evolutionary models for the donor. From both considerations, and assuming the black-hole nature for the compact object (i.e., its mass > 3M ), the possible donor mass is ≈0.5-1.4M , the inclination is ≈ 40 • -60 • and the distance is ≈8-12 kpc. The corresponding mass of the compact object is ≈4-11M . We then confirm a previous estimate that the theoretical conservative mass transfer rate in GX 339-4 is 10 −9 M yr −1 . This is 10 times lower than the average mass accretion rate estimated from the long-term X-ray light curve. We show that this discrepancy can be solved in two ways. One solution invokes irradiation of the donor by X-rays from accretion, which can temporarily enhance the mass transfer rate. We found that absorption of a ∼1 per cent of the irradiating luminosity results in the transfer rate equal to the accretion rate. The time scale at which the transfer rate will vary is estimated to be ∼10 yr, which appears consistent with the observations. The other solution invokes non-conservative mass transfer. This requires that ≈70 per cent of the transferred mass escapes as a strong outflow and carries away the specific angular momentum comparable to that of the donor.

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Section: Discussionmentioning

confidence: 78%

The X-ray binary GX 339–4/V821 Ara: the distance, inclination, evolutionary status, and mass transfer

Zdziarski

Ziółkowski

Mikołajewska

2019

Monthly Notices of the Royal Astronomical Society

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“…We choose phase bins based on the offset from the start of the obsid; this corresponds almost to the minimum in the X-ray light curve, so that we can identify our phases approximately as 0.875-0.125, 0.125-0.375, 0.375-0.625, and 0.625-0.875 We denote these in what follows as phase bins 1,2,3,4. We note that the orbital period of Cyg X-3 is increasing at a rate ofṖ /P ∼ 10 −6 yr −1 (Singh et al 2002;Bhargava et al 2017), and that the minimum of the X-ray flux occurs slightly before the phase denoted as superior conjunction, at phase 0.97 (van der Klis & Bonnet-Bidaud 1989) due to asymmetry of the light curve.…”

Section: Orbital Phase Resolved Spectramentioning

confidence: 83%

Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Kallman

McCollough

Koljonen

et al. 2019

ApJ

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We present model fits to the X-ray line spectrum of the well known High Mass X-ray binary Cyg X-3. The primary observational dataset is a spectrum taken with the Chandra X-ray Observatory High Energy Transmission Grating (HETG) in 2006, though we compare it to all the other observations of this source taken so far by this instrument. We show that the density must be ≥ 10 12 cm −3 in the region responsible for most of the emission. We discuss the influence of the dust scattering halo on the broad band spectrum and we argue that dust scattering and extinction is not the most likely origin for the narrow feature seen near the Si K edge. We identify the features of a wind in the profiles of the strong resonance lines and we show that the wind is more apparent in the lines from the lighter elements. We argue that this wind is most likely associated with the companion star. We show that the intensities of most lines can be fitted, crudely, by a single component photoionized model. However, the iron K lines do not fit with this model. We show that the iron K line variability as a function of orbital phase is different from the lower energy lines, which indicates that the lines arise in physically distinct regions. We discuss the interpretation of these results in the context of what is known about the system and similar systems.

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“…In addition to the above examples, several other publications have reported the characterization of BHXB spectral and timing properties with AstroSat science instruments, including SXT (e.g., Maqbool et al, 2019;Bhargava et al, 2019;Sreehari et al, 2019Sreehari et al, , 2020Mudambi et al, 2020b;Baby et al, 2020). SXT was also useful to probe the formation of a giant radio jet base and to measure the orbital period parameters of the X-ray binary Cygnus X-3, for which the nature of the compact object is not yet confirmed (Pahari et al, 2018b;Bhargava et al, 2017).…”

Section: Black Hole X-ray Binariesmentioning

confidence: 99%

Science with the AstroSat Soft X-ray telescope: An overview

et al. 2021

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The Soft X-ray Telescope (SXT) aboard the AstroSat satellite is the first Indian X-ray telescope in space. It is a modest size X-ray telescope with a charge coupled device (CCD) camera in the focal plane, which provides X-ray images in the ∼ 0.3 − 8.0 keV band. A forte of SXT is in providing undistorted spectra of relatively bright X-ray sources, in which it excels some current large CCD-based X-ray telescopes. Here, we highlight some of the published spectral and timing results obtained using the SXT data to demonstrate the capabilities and overall performance of this telescope.

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A Precise Measurement of the Orbital Period Parameters of Cygnus X-3

Cited by 15 publications

References 27 publications

The X-ray binary GX 339–4/V821 Ara: the distance, inclination, evolutionary status, and mass transfer

The X-ray binary GX 339–4/V821 Ara: the distance, inclination, evolutionary status, and mass transfer

Photoionization Emission Models for the Cyg X-3 X-Ray Spectrum

Science with the AstroSat Soft X-ray telescope: An overview

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