Multiwavelength observations of 1RXH J173523.7−354013: revealing an unusual bursting neutron star

Degenaar, N.; Jonker, P. G.; Torres, M. A. P.; Kaur, Ramanpreet; Rea, N.; Israel, G. L.; Patruno, A.; Trap, G.; Cackett, E.; D’Avanzo, P.; Curto, G. Lo; Novara, G.; Krimm, H. A.; Holland, S. T.; Luca, A. De; Esposito, P.; Wijnands, Rudy

doi:10.1111/j.1365-2966.2010.16388.x

Cited by 22 publications

(10 citation statements)

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“…The small orbit is required for a WD to Roche-lobe overflow such that we observe the system as an LMXB, while the lack of detected hydrogen is consistent with a WD donor. However, we reiterate that a lack of Hα does not necessarily imply a compact orbit -several LMXBs have been observed both with and without Hα emission between different epochs (see Hernández Santisteban et al (2017) for a more detailed discussion) -and a VFXB with Hα emission has been observed as well (Degenaar et al 2010). We also note that several UCXB are not very-faint X-ray binaries (Heinke et al 2013).…”

Section: Ultra-compact X-ray Binary With a White Dwarf Donor?supporting

confidence: 52%

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The very faint X-ray binary IGR J17062-6143: a truncated disc, no pulsations, and a possible outflow

Eijnden

Degenaar

Pinto

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present a comprehensive X-ray study of the neutron star low-mass X-ray binary IGR J17062-6143, which has been accreting at low luminosities since its discovery in 2006. Analysing NuSTAR, XMM-Newton and Swift observations, we investigate the very faint nature of this source through three approaches: modelling the relativistic reflection spectrum to constrain the accretion geometry, performing high-resolution X-ray spectroscopy to search for an outflow, and searching for the recently reported millisecond X-ray pulsations. We find a strongly truncated accretion disk at 77 +22 −18

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Section: Ultra-compact X-ray Binary With a White Dwarf Donor?supporting

confidence: 52%

“…Nelemans et al 2004;in't Zand et al 2009). However, Hα emission has been observed previously in a VFXB, ruling out a compact orbit as a universal explanation (Degenaar et al 2010). Furthermore, a non-detection of Hα does not necessarily imply an ultra-compact nature of the binary.…”

Section: Ultra-compact X-ray Binary With a White Dwarf Donor?mentioning

confidence: 89%

The very faint X-ray binary IGR J17062-6143: a truncated disc, no pulsations, and a possible outflow

Eijnden

Degenaar

Pinto

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…A similarly long X-ray burst has also been observed, however, from a source that accretes at 0.1 of Eddington and shows a strong H-emission line in its optical spectrum. This testifies to the presence of an H-rich companion (Degenaar et al 2010). In this case, it may be that unstable H-burning could not immediately trigger He ignition, allowing the development of a thick layer of fuel (Cooper & Narayan 2007;Peng et al 2007).…”

Section: X-ray Burst Properties Of J1850 and J1922mentioning

confidence: 98%

Two New Bursting Neutron Star Low-Mass X-Ray Binaries: Swift J185003.2-005627 and Swift J1922.7-1716

Degenaar

Linares

Altamirano

et al. 2012

ApJ

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We discuss the origin of two triggers of Swift's Burst Alert Telescope (BAT) that occurred in 2011. The triggers were identified with Swift J185003.2-005627, a previously unknown X-ray source, and the known but unclassified X-ray transient Swift J1922.7-1716. We investigate the BAT data and follow-up observations obtained with Swift's X-ray and ultraviolet/optical telescopes to demonstrate that both triggers are consistent with thermonuclear X-ray bursts. This implies that both sources are neutron star low-mass X-ray binaries. The total duration of 7 minutes and estimated energy output of (3-7) × 10 39 erg fall in between that of normal and intermediately long X-ray bursts. From the observed peaks of the X-ray bursts, we estimate a distance of 3.7 kpc for Swift J185003.2-005627 and 4.8 kpc for Swift J1922.7-1716. We characterize the outburst and quiescent X-ray properties of the two sources. They have comparable average outburst luminosities of 10 35-36 erg s −1 , and a quiescent luminosity equal to or lower than 2 × 10 32 erg s −1 (0.5-10 keV). Swift J185003.2-005627 returned to quiescence 20 d after its BAT trigger, while Swift J1922.7-1716 appears to exhibit long accretion outbursts that last several months to years. We identify a unique counterpart for Swift J1922.7-1716 in the ultraviolet/optical data. Finally, we serendipitously detect a flare lasting 500 s from an uncataloged X-ray/optical object that we tentatively classify as a flaring M-dwarf.

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“…There are other accreting systems which possess very low mass transfer rates M 10 −12 M yr −1 such as AM CVn (Solheim 2010) and even NS systems (e.g. Degenaar et al 2010), that display features of accretion e.g. emission lines, blue continuum and outbursts.…”

Section: Caveatsmentioning

confidence: 99%

The space density of post-period minimum Cataclysmic Variables

Santisteban

Knigge

Pretorius

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Binary evolution theory predicts that accreting white dwarfs with sub-stellar companions dominate the Galactic population of cataclysmic variables (CVs). In order to test these predictions, it is necessary to identify these systems, which may be difficult if the signatures of accretion become too weak to be detected. The only chance to identify such "dead" CVs is by exploiting their close binary nature. We have therefore searched the Sloan Digital Sky Survey (SDSS) Stripe 82 area for apparently isolated white dwarfs that undergo eclipses by a dark companion. We found no such eclipses in either the SDSS or Palomar Transient Factory data sets among our sample of 2264 photometrically selected white dwarf candidates within Stripe 82. This null result allows us to set a firm upper limit on the space density, ρ 0 , of dead CVs. In order to determine this limit, we have used Monte-Carlo simulations to fold our selection criteria through a simple model of the Galactic CV distribution. Assuming a T W D = 7, 500 K, the resulting 2σ limit on the space density of dead CVs is ρ 0 2 × 10 −5 pc −3 , where T W D is the typical effective temperature of the white dwarf in such systems.

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Multiwavelength observations of 1RXH J173523.7−354013: revealing an unusual bursting neutron star

Cited by 22 publications

References 50 publications

The very faint X-ray binary IGR J17062-6143: a truncated disc, no pulsations, and a possible outflow

The very faint X-ray binary IGR J17062-6143: a truncated disc, no pulsations, and a possible outflow

Two New Bursting Neutron Star Low-Mass X-Ray Binaries: Swift J185003.2-005627 and Swift J1922.7-1716

The space density of post-period minimum Cataclysmic Variables

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