Relativistic Disk Reflection in the Neutron Star X-Ray BinaryXTE J1709-267 with NuSTAR

Ludlam, R. M.; Miller, J. M.; Cackett, E.; Degenaar, N.; Bostrom, Allison

doi:10.3847/1538-4357/aa661a

Cited by 20 publications

(7 citation statements)

References 48 publications

(89 reference statements)

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“…Inner disk radii that extend a few rg away from the ISCO have often be ascribed to the presence of a geometrically thick boundary/spreading layer (e.g. D 'Aí et al, 2014;Ludlam et al, 2017a). However, in a few cases the inferred inner disk radii are so large that other explanations have been invoked.…”

Section: Accretion Disks and X-ray Spectral Statesmentioning

confidence: 99%

Accretion Disks and Coronae in the X-Ray Flashlight

et al. 2017

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Plasma accreted onto the surface of a neutron star can ignite due to unstable thermonuclear burning and produce a bright flash of X-ray emission called a Type-I X-ray burst. Such events are very common; thousands have been observed to date from over a hundred accreting neutron stars. The intense, often Eddington-limited, radiation generated in these thermonuclear explosions can have a discernible effect on the surrounding accretion flow that consists of an accretion disk and a hot electron corona. Type-I X-ray bursts can there- fore serve as direct, repeating probes of the internal dynamics of the accretion process. In this work we review and interpret the observational evidence for the impact that Type-I X-ray bursts have on accretion disks and coronae. We also provide an outlook of how to make further progress in this research field with prospective experiments and analysis techniques, and by exploiting the technical capabilities of the new and concept X-ray missions ASTROSAT, NICER, Insight-HXMT, eXTP, and STROBE-X.

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Section: Accretion Disks and X-ray Spectral Statesmentioning

confidence: 99%

Accretion Disks and Coronae in the X-Ray Flashlight

et al. 2017

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“…The strength of these effects increase with proximity to the compact object, thus allowing the position of the inner accretion disk to be determined from the shape of the Fe line profile. The accretion disk around a NS has to truncate at or prior to the surface, hence reflection studies in NS LMXBs can provide upper limits on the radial extent of these objects (Cackett et al 2008;Miller et al 2013;Ludlam et al 2017a) or indicate the presence of a boundary layer or strong magnetic field (Cackett et al 2009;Papitto et al 2009;King et al 2016;Ludlam et al 2017bLudlam et al , 2017cvan den Eijnden et al 2017).…”

Section: Introductionmentioning

confidence: 99%

NuSTAR Observations of the Accreting Atolls GX 3+1, 4U 1702-429, 4U 0614+091, and 4U 1746-371

Ludlam

Miller

Barret

et al. 2019

ApJ

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Atoll sources are accreting neutron star (NS) low-mass X-ray binaries. We present a spectral analysis of four persistent atoll sources (GX 3+1, 4U 1702−429, 4U 0614+091, and 4U 1746−371) observed for ∼ 20 ks each with NuSTAR to determine the extent of the inner accretion disk. These sources range from an apparent luminosity of 0.006 − 0.11 of the Eddington limit (assuming the empirical limit of 3.8 × 10 38 ergs s −1 ). Broad Fe emission features shaped by Doppler and relativistic effects close to the NS were firmly detected in three of these sources. The position of the disk appears to be close to the innermost stable circular orbit (ISCO) in each case. For GX 3+1, we determine R in = 1.8 +0.2 −0.6 R ISCO (90% confidence level) and an inclination of 27 • −31 • . For 4U 1702−429, we find a R in = 1.5 +1.6 −0.4 R ISCO and inclination of 53 • − 64 • . For 4U 0614+091, the disk has a position of R in = 1.3 +5.4 −0.2 R ISCO and inclination of 50 • −62 • . If the disk does not extend to the innermost stable circular orbit, we can place conservative limits on the magnetic field strength in these systems in the event that the disk is truncated at the Alfvén radius. This provides the limit at the poles of B ≤ 6.7 × 10 8 G, 3.3 × 10 8 G, and 14.5 × 10 8 G for GX 3+1, 4U 1702−429, and 4U 0614+091, respectively. For 4U 1746−371, we argue that the most plausible explanation for the lack of reflection features is a combination of source geometry and strong Comptonization. We place these sources among the larger sample of NSs that have been observed with NuSTAR.

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“…Disk truncations have been inferred in a few NS LMXBs at larger radii than in BHs at similar accretion rates, possible indeed caused by the NS magnetic fields (e.g. Tomsick et al 2009;Degenaar et al 2014;Fürst et al 2016;Iaria et al 2016;Degenaar et al 2017a;van den Eijnden et al 2017;Ludlam et al 2017b, see Appendix A for a detailed comparison. ).…”

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confidence: 96%

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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Relativistic Disk Reflection in the Neutron Star X-Ray BinaryXTE J1709-267 with NuSTAR

Cited by 20 publications

References 48 publications

Accretion Disks and Coronae in the X-Ray Flashlight

Accretion Disks and Coronae in the X-Ray Flashlight

NuSTAR Observations of the Accreting Atolls GX 3+1, 4U 1702-429, 4U 0614+091, and 4U 1746-371

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

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