Identification of a Helium Donor Star in NGC 247 ULX-1

Zhou, Changxing; Feng, Hua; Bian, Fuyan

doi:10.3847/1538-4357/acc5eb

Cited by 5 publications

(2 citation statements)

References 97 publications

(152 reference statements)

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“…For a high M He,i , BH UCXBs tend to become so-called ultraluminous X-ray sources (ULXs, L X 10 39 erg s −1 ; Feng & Soria 2011; Kaaret et al 2017), in which the maximum X-ray luminosity is 3.5 × 10 39 erg s −1 . Recently, Zhou et al (2023) found the first smoking gun evidence for the existence of He donor star in ULXs by Very Large Telescope Multi Unit Spectroscopic Explorer observations. Similarly, the population synthesis study also indicated that NS X-ray binaries containing the He stars can account for a large part of ULXs in Milky Way-like galaxies (Shao & Li 2019).…”

Section: Evolution Of X-ray Luminositiesmentioning

confidence: 99%

Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel

Qin,

Xu,

Liu

et al. 2024

ApJ

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Black hole (BH) ultracompact X-ray binaries (UCXBs) are potential Galactic low-frequency gravitational wave (GW) sources. As an alternative channel, BH UCXBs can evolve from BH+He star binaries. In this work, we perform a detailed stellar evolution model for the formation and evolution of BH UCXBs evolving from the He star channel to diagnose their detectability as low-frequency GW sources. Our calculations found that some nascent BH+He star binaries after the common-envelope (CE) phase could evolve into UCXB-LISA sources with a maximum GW frequency of ∼5 mHz, which can be detected in a distance of 10 kpc (or 100 kpc). Once BH+He star systems become UCXBs through mass transfer, they would emit X-ray luminosities of ∼1038 erg s−1, making them ideal multimessenger objects. If the initial He-star masses are ≥0.7 M ⊙, those systems are likely to experience two Roche lobe overflows, and the X-ray luminosity can reach a maximum of 3.5 × 1039 erg s−1 in the second mass-transfer stage. The initial He-star masses and initial orbital periods of progenitors of Galactic BH UCXB-LISA sources are in the range of 0.32–2.9 M ⊙ and 0.02–0.19 days, respectively. Nearly all BH+He star binaries in the above parameter space can evolve into GW sources whose chirp masses can be accurately measured. Employing a population synthesis simulation, we predict the birthrate and detection number of Galactic BH UCXB-LISA sources evolving from the He star channel are R = 2.2 × 10−6 yr−1 and 33 for an optimistic CE parameter, respectively.

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Section: Evolution Of X-ray Luminositiesmentioning

confidence: 99%

Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel

Qin,

Xu,

Liu

et al. 2024

ApJ

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“…Optical observations of ULXs may help place constraints on their compact object mass (Liu et al 2013;Motch et al 2014), accretion geometry (Vinokurov et al 2013;Ambrosi & Zampieri 2018;Yao & Feng 2019), history of binary evolution (Madhusudhan et al 2008;Patruno & Zampieri 2008;Zhou et al 2023), and interaction with the environment (e.g., Pakull & Mirioni 2002), and are thus an important probe to their physical nature. ULXs show optical emission lines reminiscent of luminous blue variables or late nitrogen Wolf-Rayet stars, or the supercritically accreting microquasar SS 433, which are all objects with powerful winds, suggesting that the optical emission lines seen in ULXs originate from a hot disk wind (Fabrika et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Identification of Bubble Nebulae around NGC 55 ULX-1 with MUSE Observations

Zhou,

Feng,

Bian

2023

ApJ

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Using the Multi Unit Spectroscopic Explorer (MUSE) instrument on the Very Large Telescope, we identified three bubble nebulae (denoted as A, B, and C) around an ultraluminous X-ray source (ULX) in NGC 55. Bubble A shows a regular elliptical shape surrounding the ULX, with a morphology similar to the canonical ULX bubble around NGC 1313 X-2. It is most likely inflated by the ULX disk wind with a mechanical power close to 1039 erg s−1. Bubble B lies 11″ away from the ULX on the sky plane and is not contiguous to Bubble A. It displays a bow-shock-like morphology, and is likely driven by a collimated dark jet from the ULX with a mechanical power of about 3 × 1038 erg s−1. If this scenario is correct, we predict that Bubble B should present radio emission with a flux of about 1–102 μJy at 5 GHz. Bubble C appears within Bubble A, with a velocity and velocity dispersion distinct from the rest of Bubble A. Its nature is unclear and could be part of Bubble A as a result of low local density. The optical counterpart of ULX-1 exhibits broad Hα, consistent with emission from a hot disk wind.

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Super-Eddington accretion as a possible scenario to form GW190425

Zhang,

Wang,

Zhu

et al. 2023

Monthly Notices of the Royal Astronomical Society

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On 2019 April 25, the LIGO/Virgo Scientific Collaboration detected a compact binary coalescence, GW190425. Under the assumption of the binary neutron star (BNS), the total mass of $3.4^{+0.3}_{-0.1}\, M_\odot$ lies five standard deviations away from the known Galactic population mean. In the standard common envelope scenario, the immediate progenitor of GW190425 is a close binary system composed of an NS and a He-rich star. With the detailed binary evolutionary modeling, we find that in order to reproduce GW190425-like events, super-Eddington accretion (e.g., $1,000\, \dot{M}_{\rm Edd}$) from a He-rich star onto the first-born NS with a typical mass of 1.33 M⊙ via stable Case BB mass transfer (MT) is necessarily required. Furthermore, the immediate progenitors should potentially have an initial mass of MZamsHe in a range of 3.0 − 3.5 M⊙ and an initial orbital period of Pinit from 0.08 days to 0.12 days, respectively. The corresponding mass accreted onto NSs via stable Case BB MT phase varies from 0.70 M⊙ to 0.77 M⊙. After the formation of the second-born NS, the BNSs are expected to be merged due to gravitational wave emission from ∼ 11 Myr to ∼ 190 Myr.

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Identification of a Helium Donor Star in NGC 247 ULX-1

Cited by 5 publications

References 97 publications

Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel

Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel

Identification of Bubble Nebulae around NGC 55 ULX-1 with MUSE Observations

Super-Eddington accretion as a possible scenario to form GW190425

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