Investigating High Mass X-ray Binaries at hard X-rays with INTEGRAL

Sidoli, L.; Paizis, A.

doi:10.1017/s1743921319001145

Cited by 3 publications

(2 citation statements)

References 18 publications

(20 reference statements)

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“…As Be XRBs are transient in nature, we included a duty cycle of 10% in our calculations (Sidoli & Paizis 2019, however see also Reig 2011 where duty cycles up to 30% are observed).…”

Section: X-ray Luminosity Calculationmentioning

confidence: 99%

X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations

Misra

Kovlakas

Fragos

et al. 2023

A&A

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Context. Many physical processes taking place during the evolution of binary stellar systems remain poorly understood. The ever-expanding observational sample of X-ray binaries (XRBs) makes them excellent laboratories for constraining binary evolution theory. Such constraints and useful insights can be obtained by studying the effects of various physical assumptions on synthetic X-ray luminosity functions (XLFs) and comparing them with observed XLFs. Aims. In this work we focus on high-mass X-ray binaries (HMXBs) and study the effects on the XLF of various, poorly constrained assumptions regarding physical processes, such as the common-envelope phase, core collapse, and wind-fed accretion. Methods. We used the new binary population synthesis code POSYDON, which employs extensive precomputed grids of detailed stellar structure and binary evolution models, to simulate the entire evolution of binaries. We generated 96 synthetic XRB populations corresponding to different combinations of model assumptions, including different prescriptions for supernova kicks, supernova remnant masses, common-envelope evolution, circularization at the onset of Roche-lobe overflow, and observable wind-fed accretion. Results. The generated HMXB XLFs are feature-rich, deviating from the commonly assumed single power law. We find a break in our synthetic XLF at luminosity ∼1038 erg s−1, similar to observed XLFs. However, we also find a general overabundance of XRBs (up to a factor of ∼10 for certain model parameter combinations) driven primarily by XRBs with black hole accretors. Assumptions about the transient behavior of Be XRBs, asymmetric supernova kicks, and common-envelope physics can significantly affect the shape and normalization of our synthetic XLFs. We find that less well-studied assumptions regarding the circularization of the orbit at the onset of Roche-lobe overflow and criteria for the formation of an X-ray-emitting accretion disk around wind-accreting black holes can also impact our synthetic XLFs and reduce the discrepancy with observations. Conclusions. Our synthetic XLFs do not always agree well with observations, especially at intermediate X-ray luminosities, which is likely due to uncertainties in the adopted physical assumptions. While some model parameters leave distinct imprints on the shape of the synthetic XLFs and can reduce this deviation, others do not have a significant effect overall. Our study reveals the importance of large-scale parameter studies, highlighting the power of XRBs in constraining binary evolution theory.

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“…As Be XRBs are transient in nature, we included a duty cycle of 10% in our calculations (Sidoli & Paizis 2019, however see also Reig 2011 where duty cycles up to 30% are observed).…”

Section: X-ray Luminosity Calculationmentioning

confidence: 99%

X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations

Misra

Kovlakas

Fragos

et al. 2023

A&A

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“…For an accreting pulsar with a long spin period such as IGR J16320-4751, magnetic field strength can be calculated in the fast rotator regime of standard accretion disk model (Ghosh & Lamb 1979). Presence of a persistent or temporary disk has been inferred in some HMXB sources like SMC X-1 (Hutchings et al 1977), LMC X-4 (Heemskerk & van Paradĳs 1989), GX 301-2 (Nabizadeh et al 2019), and OAO 1657-415 (Sidoli & Paizis 2019). The accreted matter can exert torque on the pulsar to either increase or decrease its spin, and a spin equilibrium state is arrived after multiple spin-up or spin-down episodes (Ho et al 2014).…”

Section: Hard X-ray Spectral Properties Of Igr J16320-4751mentioning

confidence: 99%

Peculiar temporal and spectral features in highly obscured HMXB pulsar IGR J16320-4751 using XMM-Newton

2023

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Comprehensive broad-band study of accreting neutron stars with Suzaku: Is there a bi-modality in the X-ray spectrum?

Pradhan

Paul

Bozzo

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a broad-band spectral analysis of accreting neutron stars using data from XIS and PIN onboard Suzaku. From spectral fits of these sources with a single continuum model including a power law and high energy cut-off, cyclotron lines (where required), we studied the correlation between various spectral parameters. Among 39 sources we studied, 16 are those where the existence of a cyclotron line is known in literature, and 29 need a cut-off energy. Among these 29 sources, 18 have cut-off energy bunched in a range of 3–10 keV while for 11 sources, it spreads over 12–25 keV. This bi-modal behaviour is not based on the specific nature of the systems being a Be XRB or supergiant HMXB, nor on different beaming patterns characterizing their X-ray emission (as inferred from simultaneous study of their pulse profiles). The broad-band coverage of Suzaku also shows that the cut-off energies saturate for higher values of cyclotron line energies – consistent with previous works in literature – for both the groups and the width of the cyclotron line show a weak correlation with the cyclotron line energy. We also find an anticorrelation with luminosity for both spectral index and folding energy, respectively. Unlike previous works, we did not detect any anticorrelation between X-ray luminosity and EW of K α lines. Finally, we show that the EW and flux of the iron K α line are smaller in SFXTs than classical NS-HMXBs. We discuss these findings in terms of different properties of stellar winds and accretion mechanisms.

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Investigating High Mass X-ray Binaries at hard X-rays with INTEGRAL

Cited by 3 publications

References 18 publications

X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations

X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations

Peculiar temporal and spectral features in highly obscured HMXB pulsar IGR J16320-4751 using XMM-Newton

Comprehensive broad-band study of accreting neutron stars with Suzaku: Is there a bi-modality in the X-ray spectrum?

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