Orbital Period and Outburst Luminosity of Transient Low Mass X-Ray Binaries

Wu, Y. X.; Yu, Wenfei; Li, T. P.; Maccarone, Tom; Li, X. D.

doi:10.1088/0004-637x/718/2/620

Cited by 74 publications

(84 citation statements)

References 75 publications

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“…Finally, the maximum luminosity that can be reached during outburst should scale with the orbital period of the binary (e.g., Lasota 2001), which is borne out by observations (e.g., Wu et al 2010). For the estimated bolometric peak X-ray luminosity of RXS J1804 (L bol ≃5 × 10 37 erg s −1 ), the empirical relation of Wu et al (2010) yields an orbital period of ≃1.4 hr.…”

Section: On the Size Of The Binary Orbitmentioning

confidence: 97%

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Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9–342058

Degenaar

Altamirano

Parker

et al. 2016

Mon. Not. R. Astron. Soc.

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ABSTRACT1RXS J180408.9-342058 is a transient neutron star low-mass X-ray binary that exhibited a bright accretion outburst in 2015. We present NuSTAR, Swift, and Chandra observations obtained around the peak brightness of this outburst. The source was in a soft X-ray spectral state and displayed an X-ray luminosity of L X ≃(2 − 3) × 10 37 (D/5.8 kpc) 2 erg s −1 (0.5-10 keV). The NuSTAR data reveal a broad Fe-K emission line that we model as relativistically broadened reflection to constrain the accretion geometry. We found that the accretion disk is viewed at an inclination of i≃27 • -35 • and extended close to the neutron star, down to R in ≃5-7.5 gravitational radii (≃11-17 km). This inner disk radius suggests that the neutron star magnetic field strength is B 2×10 8 G. We find a narrow absorption line in the Chandra/HEG data at an energy of ≃7.64 keV with a significance of ≃4.8σ. This feature could correspond to blue-shifted Fe XXVI and arise from an accretion disk wind, which would imply an outflow velocity of v out ≃0.086c (≃25 800 km s −1 ). However, this would be extreme for an X-ray binary and it is unclear if a disk wind should be visible at the low inclination angle that we infer from our reflection analysis. Finally, we discuss how the X-ray and optical properties of 1RXS J180408.9-342058 are consistent with a relatively small (P orb 3 hr) binary orbit.

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Section: On the Size Of The Binary Orbitmentioning

confidence: 97%

“…For the estimated bolometric peak X-ray luminosity of RXS J1804 (L bol ≃5 × 10 37 erg s −1 ), the empirical relation of Wu et al (2010) yields an orbital period of ≃1.4 hr. Disk instability theory predicts an orbital period of ≃2.4 hr for an irradiated He disk .…”

Section: On the Size Of The Binary Orbitmentioning

confidence: 99%

Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9–342058

Degenaar

Altamirano

Parker

et al. 2016

Mon. Not. R. Astron. Soc.

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“…These populations of extra-galactic LMXBs provide a wider observational base for the understanding of LMXB formation and evolution, which has been debated since their discovery in the Milky Way (see, e.g., Giacconi 1974;Grindlay & Henz 1985; review by Verbunt & van den Heuvel 1995;Piro & Bildsten 2002;King 2002;Bildsten & Deloye 2004). A key observational result that can constrain the nature of these LMXBs is their time variability, as luminous LMXBs (L X 10 37 erg s −1 ) in relatively wide orbits are expected to exhibit transient behavior, according to the "standard" formation scenario of LMXBs in galactic fields (Verbunt & van den Heuvel 1995;Shahbaz et al 1997;Piro & Bildsten 2002;King 2002;Wu et al 2010). For sources originating as ultracompact binaries formed in globular clusters (GCs) instead, transient behavior is only expected at lower luminosities (Bildsten & Deloye 2004).…”

Section: Introductionmentioning

confidence: 99%

The Spectral and Temporal Properties of Transient Sources in Early-Type Galaxies

Brassington¹,

Fabbiano²,

Zezas³

et al. 2012

ApJ

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We report the spectral and temporal variability properties of 18 candidate transient (TC) and potential transient (PTC) sources detected in deep multi-epoch Chandra observation of the nearby elliptical galaxies, NGC 3379, NGC 4278, and NGC 4697. Only one source can be identified with a background counterpart, leaving 17 TCs + PTCs in the galaxies. Of these, 14 are in the galaxy field, supporting the theoretical picture that the majority of field X-ray binaries (XRBs) will exhibit transient accretion for >75% of their lifetime. Three sources are coincident with globular clusters, including two high-luminosity candidate black hole (BH) XRBs, with L X = 5.4 × 10 38 erg s −1 and L X = 2.8 × 10 39 erg s −1 , respectively. The spectra, luminosities, and temporal behavior of these 17 sources suggest that the transient population is heterogeneous, including neutron star (NS) and BH XRBs in both normal and high-rate accretion modes, and super soft sources containing white dwarf binaries. Our TC and PTC detections are noticeably fewer than the number expected from the population synthesis (PS) models of Fragos et al., tailored to our new Chandra pointings of NGC 4278. We attribute this discrepancy to the PS assumption that the transient population is composed of NS XRBs, as well as differences between the statistical analysis and error estimates used in the model and our observations.

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“…Meanwhile, Wu et al (2010) found that 3−200 keV peak luminosity of XTE J1118+480 is only about 0.001 L Edd , which implied a low mass transfer rate of …”

Section: Magnetic Brakingmentioning

confidence: 99%

Orbital period decay of compact black hole X-ray binaries: the influence of circumbinary disks?

Chen

2015

A&A

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Context. Recently, compact black hole X-ray binaries XTE J 1118+480 and A0620-00 have been reported to be experiencing a fast orbital period decay, which is two orders of magnitude higher than expected with gravitational wave radiation. Magnetic braking of an Ap/Bp star has been suggested to account for the period change when the surface magnetic field of the companion star B s > ∼ 10 4 G. However, our calculation indicates that anomalous magnetic braking cannot significantly contribute to the large orbital period decay rates observed in these two sources even if B s > ∼ 10 4 G. Aims. Observations have provided evidence that circumbinary disks around two compact black hole X-ray binaries may exist. Our analysis shows that, for some reasonable parameters, tidal torque between the circumbinary disk and the binary can efficiently extract the orbital angular momentum from the binary, and result in a large orbital period change rate. Methods. Based on the circumbinary disk model, we simulate the evolution of XTE J 1118+480 via a stellar evolution code. Results. Our computations are approximatively in agreement with the observed data (the masses of two components, donor star radius, orbital period, and orbital period derivative). Conclusions. The mass transfer rate and circumbinary disk mass are obviously far greater than the inferred values from observations. Therefore, it seems that the circumbinary disk is unlikely to be the main cause of the rapid orbital decay observed in some compact black hole X-ray binaries.

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Orbital Period and Outburst Luminosity of Transient Low Mass X-Ray Binaries

Cited by 74 publications

References 75 publications

Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9–342058

Disc reflection and a possible disc wind during a soft X-ray state in the neutron star low-mass X-ray binary 1RXS J180408.9–342058

The Spectral and Temporal Properties of Transient Sources in Early-Type Galaxies

Orbital period decay of compact black hole X-ray binaries: the influence of circumbinary disks?

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