Evolution of LMXBs under Different Magnetic Braking Prescriptions

Deng, Zhu-Ling; Li, Xiangdong; Gao, Zhi‐Fu; Shao, Yong

doi:10.3847/1538-4357/abe0b2

Cited by 54 publications

(29 citation statements)

References 64 publications

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“…where 𝛾 mb ∼ 0 − 4 is the magnetic braking parameter (in our calculations we take the default value 𝛾 mb = 3); Ω is the orbital angular velocity, 𝑅 d is the radius of the donor star; 𝜏 c is the turnover time of the convective eddies of the donor star and 𝜏 2.8 × 10 6 s is the turnover time of the Sun; 𝜉 mb is the convection-boosted power low index and we take 𝜉 mb = 2 ( Van et al 2019;Deng et al 2021). The convection-boosted magnetic braking model is based on the widely-used traditional magnetic braking model (Rappaport et al 1983) by adding a boosting factor 𝜏 c .…”

Section: Evolution Of Ns I/lmxbsmentioning

confidence: 99%

“…Van et al (2019) found that this model is able to reproduce some particular NS LMXBs. Deng et al (2021) systematically compared five types of magnetic braking prescriptions in the literature, and found that the convection-boosted model seems to be more suitable to account for the overall properties of LMXBs, compared with other magnetic braking prescriptions.…”

Section: Evolution Of Ns I/lmxbsmentioning

confidence: 99%

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Formation of Mass-gap Black Holes from Neutron Star X-ray Binaries with Super-Eddington Accretion

Gao,

Li,

Shao

2022

Preprint

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Electromagnetic and gravitational wave observations indicate that there is dearth of compact objects with mass ∼ 2.5 − 5 M . This so-called "mass gap" may be linked to the supernova explosion mechanisms that produce neutron stars (NSs) and black holes (BHs). However, the existence of a few mass-gap compact objects, some of which have been confirmed to be BHs, poses a challenge to the traditional theory of black hole formation. In this work we investigate the possible formation channel of BHs from accretion-induced collapse (AIC) of NSs in X-ray binaries. In particular, we consider the influence of super-Eddington accretion of NSs. Recent observations of ultraluminous X-ray pulsars suggest that their apparent luminosities may reflect the true accretion luminosities of the accreting NSs, even exceeding the Eddington limit by a factor of 100. Thus, NSs accreting at a super-Eddington accretion rate may rapidly grow into BHs in intermediate/low-mass X-ray binaries. Based on the super-Eddington accretion disk models, we have investigated the evolution of NSs in intermediate/low-mass X-ray binaries by combining binary population synthesis and detailed stellar evolutionary calculations. We show that super-Eddington accretion plays a critical role in mass growth of NSs, and the final masses of the descendant BHs are heavily dependent on the NS magnetic fields, the metallicity of the donor star, and the bifurcation period of the binaries. AIC of NSs may account for some of the observed mass-gap BHs like GRO J0422+32. We also present the parameter distributions of the potential mass-gap BHs in a Milky Way-like galaxy, and point out that future space-based gravitational wave observations may provide important test of or constraints on the formation of mass-gap BHs from the AIC channel.

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Section: Evolution Of Ns I/lmxbsmentioning

confidence: 99%

Section: Evolution Of Ns I/lmxbsmentioning

confidence: 99%

Formation of Mass-gap Black Holes from Neutron Star X-ray Binaries with Super-Eddington Accretion

Gao,

Li,

Shao

2022

Preprint

Self Cite

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“…Recent astronomical studies have revealed that the magnetic fields are crucial for the origin and evolution of different astrophysical systems such as solar flares, fast radio burst, binary systems, Gamma-ray pulsars, magnetars, active galactic nuclei jets, galaxy-cluster evolution etc. [7][8][9][10][11]. Consequently different varieties of cosmological processes also can produce relatively high primordial magnetic fields of strength 10 −10 − 10 −9 gauss at the redshift z ∼ 5 [6].…”

Section: Introductionmentioning

confidence: 99%

Density perturbation and cosmological evolution in the presence of magnetic field in $f(R)$ gravity models

Chakraborty¹,

Guha²

2021

Preprint

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In this paper, we have investigated the density perturbations and cosmological evolution in the FLRW universe in presence of a cosmic magnetic field, which may be assumed to mimic primordial magnetic fields. Such magnetic fields have sufficient strength to influence galaxy formation and cluster dynamics, thereby leaving an imprint on the CMB anisotropies. We have considered the FLRW universe as a representative of the isotropic cosmological model in the 1+3 covariant formalism for f (R) gravity. The propagation equations have been determined and analyzed, where we have assumed that the magnetic field is aligned uniformly along the x-direction, resulting in a diagonal shear tensor. Subsequently,the density perturbation evolution equations have been studied and the results have been interpreted. We have also indicated how these results change in the general relativistic case and briefly mentioned the expected change in higher-order gravity theories.

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“…It has been suggested that the bifurcation period is sensitive to the angular-momentum loss mechanisms, especially the magnetic braking laws and the mass-loss prescriptions (e.g. Ergma 1996;Podsiadlowski, Rappaport & Pfahl 2002;Ma & Li 2009a;Shao & Li 2015;Chen et al 2017;Deng et al 2021). It is worth noting that part of the current LMXBs may originate from the evolution of intermediate-mass X-ray binaries (IMXBs) that appear as LMXBs in most of their X-ray active lifetime (e.g.…”

Section: Introductionmentioning

confidence: 99%

Ultra-compact X-ray binaries with He star companions

Wang,

Chen,

Liu

et al. 2021

Preprint

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Ultra-compact X-ray binaries (UCXBs) are low-mass X-ray binaries with hydrogen-deficient mass-donors and ultra-short orbital periods. They have been suggested to be the potential Laser Interferometer Space Antenna (LISA) sources in the low-frequency region. Several channels for the formation of UCXBs have been proposed so far. In this article, we carried out a systematic study on the He star donor channel, in which a neutron star (NS) accretes matter from a He main-sequence star through Roche-lobe overflow, where the mass-transfer is driven by the gravitational wave radiation. Firstly, we followed the long-term evolution of the NS+He main-sequence star binaries by employing the stellar evolution code Modules for Experiments in Stellar Astrophysics, and thereby obtained the initial parameter spaces for the production of UCXBs. We then used these results to perform a detailed binary population synthesis approach to obtain the Galactic rates of UCXBs through this channel. We estimate the Galactic rates of UCXBs appearing as LISA sources to be ∼ 3.1 − 11.9 × 10 −6 yr −1 through this channel, and the number of such UCXB-LISA sources in the Galaxy can reach about 100 − 390. The present work indicates that the He star donor channel cannot be ignored in forming UCXB-LISA sources. We found that the evolutionary tracks of UCXBs through this channel can account for the location of the five transient sources with relatively long orbital periods quite well. We also found that such UCXBs can be identified by their locations in the period-mass transfer rate diagram.

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Evolution of LMXBs under Different Magnetic Braking Prescriptions

Cited by 54 publications

References 64 publications

Formation of Mass-gap Black Holes from Neutron Star X-ray Binaries with Super-Eddington Accretion

Formation of Mass-gap Black Holes from Neutron Star X-ray Binaries with Super-Eddington Accretion

Density perturbation and cosmological evolution in the presence of magnetic field in $f(R)$ gravity models

Ultra-compact X-ray binaries with He star companions

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