Tidal interaction in High‐Mass X‐ray Binaries

Stoyanov, K. A.; Zamanov, R.

doi:10.1002/asna.200811224

Cited by 9 publications

(9 citation statements)

References 39 publications

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“…Second, we also assume that the orbit has already been approximately circularized by tidal forces. The latter assumption is supported by the analytic solutions of Zahn (1975) and Hurley et al (2002), and their application to high-mass XRBs (Stoyanov & Zamanov 2009), which show that both BH and NS systems with a donor star mass M2 10M⊙ and a binary period P 10 d will circularize in 10 6 yrs, while systems with longer periods (usually including Be XRBs) may not circularize. Since S2 has a binary period ≈2.2 days, and a likely massive donor mass (as we discussed in Section 6), our assumption of tidal circularization is reasonable.…”

Section: Photometric Identification Of An Accreting Ns In S2mentioning

confidence: 88%

Discovery of two eclipsing X-ray binaries in M 51

Wang

Soria

Urquhart

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We discovered eclipses and dips in two luminous (and highly variable) X-ray sources in M 51. One (CXOM51 J132943.3+471135) is an ultraluminous supersoft source, with a thermal spectrum at a temperature of about 0.1 keV and characteristic blackbody radius of about 10 4 km. The other (CXOM51 J132946.1+471042) has a two-component spectrum with additional thermal-plasma emission; it approached an X-ray luminosity of 10 39 erg s −1 during outbursts in 2005 and 2012. From the timing of three eclipses in a series of Chandra observations, we determine the binary period (52.75 ± 0.63 hr) and eclipse fraction (22% ± 0.1%) of CXOM51 J132946.1+471042. We also identify a blue optical counterpart in archival Hubble Space Telescope images, consistent with a massive donor star (mass of ∼20-35M ⊙ ). By combining the X-ray lightcurve parameters with the optical constraints on the donor star, we show that the mass ratio in the system must be M 2 /M 1 18, and therefore the compact object is most likely a neutron star (exceeding its Eddington limit in outburst). The general significance of our result is that we illustrate one method (applicable to high-inclination sources) of identifying luminous neutron star X-ray binaries, in the absence of X-ray pulsations or phase-resolved optical spectroscopy. Finally, we discuss the different Xray spectral appearance expected from super-Eddington neutron stars and black holes at high viewing angles.

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Section: Photometric Identification Of An Accreting Ns In S2mentioning

confidence: 88%

Discovery of two eclipsing X-ray binaries in M 51

Wang

Soria

Urquhart

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…In Fig. 5 we plot P rot versus P orb for a number of high-mass X-ray binaries (see also Stoyanov & Zamanov 2009). Highmass X-ray binaries with a giant/supergiant component, Be/Xray binaries, and Be/γ-ray binaries are plotted with different symbols in this figure.…”

Section: Rotational Period Of the Mass Donorsmentioning

confidence: 99%

Optical spectroscopy of Be/gamma-ray binaries

Zamanov

Stoyanov

Martı́

et al. 2016

A&A

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We report optical spectroscopic observations of the Be/γ-ray binaries LSI+61303, MWC 148 and MWC 656. The peak separation and equivalent widths of prominent emission lines (Hα, Hβ, Hγ, HeI, and FeII) are measured. We estimated the circumstellar disc size, compared it with separation between the components, and discussed the disc truncation. We find that in LSI+61• 303 the compact object comes into contact with the outer parts of the circumstellar disc at periastron, in MWC 148 the compact object goes deeply into the disc during the periastron passage, and in MWC 656 the black hole is accreting from the outer parts of the circumstellar disc along the entire orbit. The interstellar extinction was estimated using interstellar lines. The rotation of the mass donors appears to be similar to the rotation of the mass donors in Be/X-ray binaries. We suggest that X-ray/optical periodicity ∼1 day deserves to be searched for.

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“…The long orbital periods and high eccentricities inferred for the system are therefore consistent with the Binder et al(2016) interpretation of SN2010da as a newly formed HMXB. Circularization timescales estimated for known sgHMXBs range from ∼10 4 -10 7 years (Stoyanov & Zamanov 2009), which suggests that the presumed HMXB associated with SN2010da is less than 10 4 years old. We can glean insight on the orbital and disk/shell configuration of the system from the upper limit derived for the semimajor axis of the binary.…”

Section: An Lbv or Sgb[e] Hmxb?mentioning

confidence: 99%

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

Lau

Kasliwal

Bond

et al. 2016

ApJ

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We present multi-epoch mid-infrared (IR) photometry and the optical discovery observations of the "impostor" supernova (SN) 2010da in NGC300 using new and archival Spitzer Space Telescope images and ground-based observatories. The mid-infrared counterpart of SN2010da was detected as Spitzer Infrared Intensive Transient Survey (SPIRITS)14bme in the SPIRITS, an ongoing systematic search for IR transients. Before erupting on 2010 May 24, the SN2010da progenitor exhibited a constant mid-IR flux at 3.6 and only a slight ∼10% decrease at 4.5 μm between 2003 November and 2007 December. A sharp increase in the 3.6 μm flux followed by a rapid decrease measured ∼150 days before and ∼80 days after the initial outburst, respectively, reveal a mid-IR counterpart to the coincident optical and high luminosity X-ray outbursts. At late times, after the outburst (∼2000 days), the 3.6 and 4.5 μm emission increased to over a factor of twotimes the progenitor flux and is currently observed (as of 2016 Feb) to be fading, but still above the progenitor flux. We attribute the re-brightening mid-IR emission to continued dust production and increasing luminosity of the surviving system associated with SN2010da. We analyze the evolution of the dust temperature (T d ∼700-1000 K), mass (M d ∼0.5-3.8×10 −7 M e ), luminosity (L IR ∼1.3-3.5×10 4 L e ), and the equilibrium temperature radius (R eq ∼6.4-12.2 au) in order to resolve the nature of SN2010da. We address the leading interpretation of SN2010da as an eruption from a luminous blue variable high-mass X-ray binary (HMXB) system. We propose that SN2010da is instead a supergiant (sg)B[e]-HMXB based on similar luminosities and dust masses exhibited by two other known sgB[e]-HMXB systems. Additionally, the SN2010da progenitor occupies a similar region on a mid-IR color-magnitude diagram (CMD) with known sgB[e] stars in the Large Magellanic Cloud. The lower limit estimated for the orbital eccentricity of the sgB[e]-HMXB (e>0.82) from X-ray luminosity measurements is high compared to known sgHMXBs and supports the claim that SN2010da may be associated with a newly formed HMXB system.

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Tidal interaction in High‐Mass X‐ray Binaries

Cited by 9 publications

References 39 publications

Discovery of two eclipsing X-ray binaries in M 51

Discovery of two eclipsing X-ray binaries in M 51

Optical spectroscopy of Be/gamma-ray binaries

RISING FROM THE ASHES: MID-INFRARED RE-BRIGHTENING OF THE IMPOSTOR SN 2010da IN NGC 300

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