Thermal timescale mass transfer rates in intermediate-mass  
X-ray binaries

Xu, Xiaojie; Li, Xiangdong

doi:10.1051/0004-6361:20077637

Cited by 5 publications

(4 citation statements)

References 21 publications

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“…Investigation by Xu & Li [34] on (sub) thermal mass transfer in IMXBs shows that in most cases an NS can accrete a ≤0.1 M⊙ mass rapidly during this phase. Thisamount of mass is able to decrease the neutron star's magnetic fields down to ~10 8 −10 9 G, and spin the star up to milliseconds.…”

Section: Resultsmentioning

confidence: 99%

The low-mass X-ray binary-millisecond radio pulsar birthrate problem revisited

Dai

2010

Sci. China Phys. Mech. Astron.

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We investigate the birthrate problem for low-mass X-ray binaries (LMXBs) and millisecond radio pulsars (MRPs) in this paper. We consider intermediate-mass and low-mass X-ray binaries (I/LMXBs) to be the progenitors of MRPs, and calculate their evolutionary response to the cosmic star formation rate (SFR) both semi-analytically and numerically. With a typical value (1 Gyr) of the LMXB lifetime, one may expect comparable birthrates of LMXBs and MRPs, but the calculated number of LMXBs is an order of magnitude higher than that observed in the Galaxy. Instead, we suggest that the birthrate problem could be solved if most MRPs have evolved from faint to rather than bright LMXBs. The former may have a population of 10 4 in the Galaxy.close binaries, general pulsars, star formation, X-ray stars

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Section: Resultsmentioning

confidence: 99%

The low-mass X-ray binary-millisecond radio pulsar birthrate problem revisited

Dai

2010

Sci. China Phys. Mech. Astron.

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“…A plausible scenario for BH LMXBs with high spin parameters is that, at the initial stage of the XRB phase, the system is required to be an intermediate-mass X-ray binary (IMXB) with a comparable companion mass to the BH (𝑞 ∼ 1), and then the companion star must lose most of its mass to feed the BH. It is expected that a BH IMXB experiences a period with hypercritical accretion rate (≫ 𝑀 Edd ) due to the thermal timescale mass transfer (∼ 10 −6 -10 −5 𝑀 ⊙ /𝑦𝑟), when the BH accretes large amounts of mass during a short duration (∼ a few Myr) (Podsiadlowski et al 2002;Xu & Li 2007). Some ultraluminous X-ray sources (ULXs) in external galaxies are possibly such IMXBs, which are evolving towards to BH LMXBs (King et al 2000(King et al , 2001Kalogera et al 2004;Begelman et al 2006;King & Nixon 2016).…”

Section: Bh Xrbsmentioning

confidence: 99%

An apparent positive relation between spin and orbital angular momentum in X-ray binaries

Yan

Zhang

2023

Monthly Notices of the Royal Astronomical Society

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The origin of current angular momentum (AM) of the black hole (BH) in X-ray binary (XRB) is still unclear, which is related with the birth and/or the growth of the BH. Here we collect the spin parameters a* measured in BH XRBs and find an apparent bimodal distribution centered at ∼ 0.17 and 0.83. We find a positive relation between the spin parameter and the orbital period/orbital separation through combining distinct XRB categories, including neutron star (NS) low-mass X-ray binaries (LMXBs), Roche-lobe overflow (RLOF) BH XRBs and wind-fed BH XRBs. It seems that the AM of the compact star and the binary orbit correlates by combining the different XRB systems. These positive relations imply that accretion process is a common mechanism for spinning up the compact star in these diverse XRB systems. We infer that the low and high spin BH XRBs may experience different evolution and accretion history, which corresponds to the bimodal distribution of the BH spin parameters. The low spin BHs (a* < 0.3) are similar to the NS LMXBs, the compact star of which is spun-up by the low-level accretion, and the high spin BHs (a* > 0.5) had experienced a short hypercritical accretion ($\gg \dot{M}_\mathrm{Edd}$) period, during which, the BH spin dramatically increased.

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“…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. Podsiadlowski, Rappaport & Pfahl 2002;Li 2002Li , 2015Xu & Li 2007;Lin et al 2011;Shao & Li 2012). Chen & Podsiadlowski (2016) argued that the pre-IMXBs with initial orbital periods much near the bifurcation period can evolve towards UCXBs via the magnetic braking caused by the coupling between the magnetic field and an irradiationdriven wind.…”

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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Thermal timescale mass transfer rates in intermediate-mass X-ray binaries

Cited by 5 publications

References 21 publications

The low-mass X-ray binary-millisecond radio pulsar birthrate problem revisited

The low-mass X-ray binary-millisecond radio pulsar birthrate problem revisited

An apparent positive relation between spin and orbital angular momentum in X-ray binaries

Ultra-compact X-ray binaries with He star companions

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