Are There Magnetars in High-mass X-Ray Binaries?*

Xu, Kun; Li, Xiangdong; Cui, Zhe; Li, Qiaochu; Shao, Yong; Liang, Xian-Ting; Liu, Jifeng

doi:10.1088/1674-4527/ac321f

Cited by 6 publications

(2 citation statements)

References 107 publications

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“…a v oiding rapid magnetic field decay) in certain accreting systems (Igoshev & Popov 2018 ;Bozzo et al 2022 ). F or e xample, the orbital and spin periods measured for 2SXPS J075542.5-293353 agree with the magnetar X-ray binary model predictions of Xu et al ( 2021 ). Unfortunately, we cannot compare the age of the magnetar in this system with an estimated age of the star, because the P / Ṗ age becomes unreliable in an accreting system.…”

Section: Sgr0755mentioning

confidence: 79%

Where are the magnetar binary companions? Candidates from a comparison with binary population synthesis predictions

Chrimes

Levan

Fruchter

et al. 2022

Monthly Notices of the Royal Astronomical Society

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It is well established that magnetars are neutron stars with extreme magnetic fields and young ages, but the evolutionary pathways to their creation are still uncertain. Since most massive stars are in binaries, if magnetars are a frequent result of core-collapse supernovae, some fraction are expected to have a bound companion at the time of observation. In this paper, we utilize literature constraints, including deep Hubble Space Telescope imaging, to search for bound stellar companions to magnetars. The magnitude and colour measurements are interpreted in the context of binary population synthesis predictions. We find two candidates for stellar companions associated with CXOU J171405.7–381031 and SGR 0755–2933, based on their J-H colours and H-band absolute magnitudes. Overall, the proportion of the Galactic magnetar population with a plausibly stellar near-infrared counterpart candidate, based on their magnitudes and colours, is between 5 and 10 per cent. This is consistent with a population synthesis prediction of 5 per cent, for the fraction of core-collapse neutron stars arising from primaries which remain bound to their companion after the supernova. These results are therefore consistent with magnetars being drawn in an unbiased way from the natal core-collapse neutron star population, but some contribution from alternative progenitor channels cannot be ruled out.

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Section: Sgr0755mentioning

confidence: 79%

Where are the magnetar binary companions? Candidates from a comparison with binary population synthesis predictions

Chrimes

Levan

Fruchter

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Unfortunately, the errors are too large to provide a meaningful constraint since the line flux ratio of 0.7 ± 0.4 essentially spans the entire ratio range for the sample of IPs studied by Xu et al ( 2019 ). It is explained in Yu, Xu & Li ( 2022 ) that the iron line ratio method for determining WD masses has limitations at the high-mass end due to the thermal plasma model used and the fact that the most massive WD in their sample has a mass of 1.2 M .…”

Section: Discussion a N D C O N C L U S I O N Smentioning

confidence: 99%

Classifying IGR J15038−6021 as a magnetic CV with a massive white dwarf

Tomsick

Kumar

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Cataclysmic variables (CVs) are binary systems consisting of a white dwarf (WD) accreting matter from a companion star. Observations of CVs provide an opportunity to learn about accretion disks, the physics of compact objects, classical novae, and the evolution of the binary and the WD that may ultimately end in a type Ia supernova (SN). As type Ia SNe involve a WD reaching the Chandrasekhar limit or merging WDs, WD mass measurements are particularly important for elucidating the path from CV to type Ia SN. For intermediate polar (IP) type CVs, the WD mass is related to the bremsstrahlung temperature of material in the accretion column, which typically peaks at X-ray energies. Thus, the IPs with the strongest hard X-ray emission, such as those discovered by the INTEGRAL satellite, are expected to have the highest masses. Here, we report on XMM-Newton, NuSTAR, and optical observations of IGR J15038–6021. We find an X-ray periodicity of 1678 ± 2 s, which we interpret as the WD spin period. From fitting the 0.3-79 keV spectrum with a model that uses the relationship between the WD mass and the post-shock temperature, we measure a WD mass of $1.36^{+0.04}_{-0.11}$ $M_{\mathord \odot }$. This follows an earlier study of IGR J14091–6108, which also has a WD with a mass approaching the Chandrasekhar limit. We demonstrate that these are both outliers among IPs in having massive WDs and discuss the results in the context of WD mass studies as well as the implications for WD mass evolution.

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Probing the emission mechanism and nature of the pulsating compact object in the X-ray binary SAX J1324.4−6200

Ducci,

Bozzo,

Burgay

et al. 2024

A&A

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Recently, there has been renewed interest in the Be X-ray binary (Be/XRB) because of its spatial coincidence with a variable gamma -ray source detected by To explore more thoroughly its properties, new X-ray observations were carried out in 2023 by and satellites, jointly covering the energy range from $0.2-79$ keV. was caught at an X-ray flux of $ $ erg cm$^ $ s$^ $. The X-ray spectrum fits well with an absorbed power law with a high energy cutoff. Other acceptable fits require an additional blackbody component ($kT_ bb 1.1$ keV) or a Gaussian in absorption gabs keV). We measured a spin period of $175.8127 and an spin period of $175.862 We show that all the available spin period measurements of spanning 29 years, are highly correlated with time, resulting in a remarkably stable spin-down of $ P $ s s$^ $. We find that if hosts an accretion-powered pulsar, accretion torque models indicate a surface magnetic field of $ $ G. The X-ray properties emerging from our analysis strenghten the hypothesis that belongs to the small group of persistent Be/XRBs. We also performed radio observations with the Parkes Murriyang telescope, to search for radio pulsations. However, no radio pulsations compatible with the rotational ephemeris of were detected. We rule out the hypothesis that is a gamma -ray binary where the emission is produced by interactions between the pulsar and the companion winds. Other models commonly used to account for the production of $ in accreting pulsars cannot reproduce the bright emission from We examined other possible mechanisms behind the $ emission and note that there is a $ 0.5$<!PCT!> chance probability that an unknown extragalactic active galactic nucleus (AGN) observed through the Galactic plane may coincidentally fall within the error circle of the source and be responsible for the $ emission.

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Are There Magnetars in High-mass X-Ray Binaries?*

Cited by 6 publications

References 107 publications

Where are the magnetar binary companions? Candidates from a comparison with binary population synthesis predictions

Where are the magnetar binary companions? Candidates from a comparison with binary population synthesis predictions

Classifying IGR J15038−6021 as a magnetic CV with a massive white dwarf

Probing the emission mechanism and nature of the pulsating compact object in the X-ray binary SAX J1324.4−6200

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