Infrared Spectroscopy of Symbiotic Stars. XII. The Neutron Star SyXB System 4U 1700+24 = V934 Herculis

Hinkle, Kenneth H.; Fekel, Francis C.; Joyce, R. R.; Mikołajewska, Joanna; Gałan, C.; Lebzelter, T.

doi:10.3847/1538-4357/aafba5

Cited by 23 publications

(13 citation statements)

References 90 publications

(148 reference statements)

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“…It is thus possible that the enhancement in the mass accretion rate that was needed by IGR J17329−2731 to finally turn on as a SyXB has been caused by the NS interaction with one (or more) large stellar wind clump. If the orbit of the system is as large (or larger) than that measured for 4U 1700+24 (Hinkle et al 2019), then we might conclude that in the past the NS has never being in contact with similarly large structures and thus no X-ray emission could ever be detected before 2017. According to this scenario, it is possible that IGR J17329−2731 will stop shining in X-rays over the time scale of one to few years, as soon as the orbit of the compact object does no longer intersect a massive stellar wind clump.…”

Section: Igr J17329−2731mentioning

confidence: 87%

“…The source shows a remarkable variability in X-rays, achieving a total dynamic range of at least ∼200, considering also that the source has been detected undergoing short outbursts a few times by both Swift and MAXI (Kennea et al 2014;Fukushima et al 2014;Burrows et al 2014Burrows et al , 2015. The M giant companion is relatively well studied and it has been recently reported though long-term optical and near-IR observations the discovery of its pulsating period (about 420 days), as well as the orbital period of the system measured at ∼12.0 years (Hinkle et al 2019). This is by far the longest known orbital period for a SyXB and the detailed modeling of the optical data provided support in favor of the previous finding that the system is observed pole-on, with an estimated orbital inclination of 11.3±0.4 • .…”

Section: Introductionmentioning

confidence: 99%

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The Symbiotic X-ray binaries Sct X-1, 4U 1700+24 and IGR J17329-2731

Bozzo,

Romano,

Ferrigno

et al. 2022

Preprint

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Symbiotic X-ray binaries are systems hosting a neutron star accreting form the wind of a late type companion. These are rare objects and so far only a handful of them are known. One of the most puzzling aspects of the symbiotic X-ray binaries is the possibility that they contain strongly magnetized neutron stars. These are expected to be evolutionary much younger compared to their evolved companions and could thus be formed through the (yet poorly known) accretion induced collapse of a white dwarf. In this paper, we perform a broad-band X-ray and soft γ-ray spectroscopy of two known symbiotic binaries, Sct X−1 and 4U 1700+24, looking for the presence of cyclotron scattering features that could confirm the presence of strongly magnetized NSs. We exploited available Chandra, Swift, and NuSTAR data. We find no evidence of cyclotron resonant scattering features (CRSFs) in the case of Sct X−1 but in the case of 4U 1700+24 we suggest the presence of a possible CRSF at ∼16 keV and its first harmonic at ∼31 keV, although we could not exclude alternative spectral models for the broad-band fit. If confirmed by future observations, 4U 1700+24 could be the second symbiotic X-ray binary with a highly magnetized accretor. We also report about our long-term monitoring of the last discovered symbiotic X-ray binary IGR J17329−2731 performed with Swift/XRT. The monitoring revealed that, as predicted, in 2017 this object became a persistent and variable source, showing X-ray flares lasting for a few days and intriguing obscuration events that are interpreted in the context of clumpy wind accretion.

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Section: Igr J17329−2731mentioning

confidence: 87%

Section: Introductionmentioning

confidence: 99%

The Symbiotic X-ray binaries Sct X-1, 4U 1700+24 and IGR J17329-2731

Bozzo,

Romano,

Ferrigno

et al. 2022

Preprint

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“…Hinkle et al 2006;I lkiewicz, Miko lajewska & Monard 2017). (2) 4U 1700+24=V934 Her hosts a pulsar with an orbital period of ∼12 yr, and the photospheric abundances with no trace of the NS-forming supernova event indicate that it is likely a post-AIC system (see Hinkle et al 2019). In both systems, the RG donors are evolving towards the asymptotic giant branch, increasing the mass-transfer rate.…”

Section: Post-aic Systemsmentioning

confidence: 99%

Formation of millisecond pulsars with long orbital periods by accretion-induced collapse of white-dwarfs

Wang,

Liu,

Chen

2022

Preprint

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Accretion-induced collapse (AIC) of massive white-dwarfs (WDs) has been proposed as an important way for the formation of neutron star (NS) systems. An oxygen-neon (ONe) WD that accretes H-rich material from a red-giant (RG) star may experience the AIC process, eventually producing millisecond pulsars (MSPs), known as the RG donor channel. Previous studies indicate that this channel can only account for MSPs with orbital periods > 500 d. It is worth noting that some more MSPs with wide orbits (60−500 d) have been detected by recent observations, but their origin is still highly uncertain. In the present work, by employing an adiabatic power-law assumptions for the mass-transfer process, we performed a large number of complete binary evolution calculations for the formation of MSPs through the RG donor channel in a systematic way. We found that this channel can contribute to the observed MSPs with orbital periods in the range of 50 − 1200 d, and almost all the observed MSPs with wide orbits can be covered by this channel in the WD companion mass versus orbital period diagram. The present work indicates that the AIC process provides a viable way to form MSPs with wide orbits.

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“…The MAP sample parameters are reported in Table 1, with errors given by the standard deviation of the MCMC samples. The few RVs at phase ∼ 0.6 that do not agree with the modeled Keplerian orbit are potentially representative of additional RV variability due to a flare or pulsation of the RG component (e.g., Hinkle et al 2019); however, there is no existing well-cadenced (i.e., observations every few days), infrared photometry that overlaps this phase in the binary orbit to confirm the occurrence of a flare.…”

Section: Radial Velocity Analysismentioning

confidence: 99%

Geometry of the Draco C1 Symbiotic Binary

Lewis,

Anguiano,

Stassun

et al. 2020

Preprint

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Draco C1 is a known symbiotic binary star system composed of a carbon red giant and a hot, compact companion -likely a white dwarf -belonging to the Draco dwarf spheroidal galaxy. From near-infrared spectroscopic observations taken by the Apache Point Observatory Galactic Evolution Experiment (APOGEE-2), part of Sloan Digital Sky Survey IV, we provide updated stellar parameters for the cool, giant component, and constrain the temperature and mass of the hot, compact companion. Prior measurements of the periodicity of the system, based on only a few epochs of radial velocity data or relatively short baseline photometric observations, were sufficient only to place lower limits on the orbital period (P > 300 days). For the first time, we report precise orbital parameters for the binary system: With 43 radial velocity measurements from APOGEE spanning an observational baseline of more than 3 years, we definitively derive the period of the system to be 1220.0 +3.7 −3.5 days. Based on the newly derived orbital period and separation of the system, together with estimates of the radius of the red giant star, we find that the hot companion must be accreting matter from the dense wind of its evolved companion.

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Infrared Spectroscopy of Symbiotic Stars. XII. The Neutron Star SyXB System 4U 1700+24 = V934 Herculis

Abstract: V934 Her = 4U 1700+24 is an M giant-neutron star (NS) X-ray symbiotic (SyXB) system. Employing optical and infrared radial velocities spanning 29 years combined with the extensive velocities in the literature, we compute the spectroscopic orbit of

Cited by 23 publications

References 90 publications

The Symbiotic X-ray binaries Sct X-1, 4U 1700+24 and IGR J17329-2731

The Symbiotic X-ray binaries Sct X-1, 4U 1700+24 and IGR J17329-2731

Formation of millisecond pulsars with long orbital periods by accretion-induced collapse of white-dwarfs

Geometry of the Draco C1 Symbiotic Binary

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