Neutron star black hole binaries in LIGO/Virgo O3b run were formed from Population I/II binaries

Kinugawa, Tomoya; Nakamura, Takashi; Nakano, Hiroyuki

doi:10.48550/arxiv.2201.06713

Cited by 4 publications

(7 citation statements)

References 33 publications

(38 reference statements)

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“…With an effective inspiral spin of χ eff = 0.60 +0.26 −0.07 , this event could be a potential NSBH merger with the NS first born. Román-Garza et al (2021) claimed that the fraction of the NS-first-born systems with different SN engines is ∼ 10% (see also Kinugawa et al 2022). The event rate and system parameter distribution for NS-first-born NSBH mergers are subject to further studies in the future.…”

Section: Conclusion and Discussionmentioning

confidence: 94%

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A Channel to Form Fast-spinning Black Hole--Neutron Star Binary Mergers as Multi-messenger Sources

Hu,

Zhu,

Qin

et al. 2022

Preprint

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After the successful detection of a gravitational-wave (GW) signal and its associated electromagnetic (EM) counterparts from GW170817, neutron star-black hole (NSBH) mergers have been highly expected to be the next type of multi-messenger source. However, despite the detection of several of NSBH merger candidates during the GW third observation run, no confirmed EM counterparts from these sources have been identified. The most plausible explanation is that these NSBH merger candidates were plunging events mainly because the primary BHs had near-zero projected aligned-spins based on GW observations. In view that NSs can be easily tidally disrupted by BHs with high projected aligned-spins, we study an evolution channel to form NSBH binaries with fast-spinning BHs, the properties of BH mass and spin, and their associated tidal disruption probability. We find that if the NSs are born firstly, the companion helium stars would be tidally spun up efficiently, and would thus finally form fast-spinning BHs. If BHs do not receive significant natal kicks at birth, these NSBH binaries that can merge within the Hubble time would have BHs with the projected aligned-spins χ z 0.8 and, hence, can certainly allow tidal disruption to happen. Even if significant BH kicks are considered for a small fraction of NSBH binaries, the projected aligned-spins of BHs are χ z 0.2. These systems can still be disrupted events unless the NSs are very massive. Thus, NS-first-born NSBH mergers would be promising multi-messenger sources. We discuss various potential EM counterparts associated with these systems and their detectability in the upcoming fourth observation run.

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Section: Conclusion and Discussionmentioning

confidence: 94%

“…Corresponding median values of MNS for these two sources are marked as dashed lines. Both GW200105 and GW200115, which are believed to form via the BH-first-born formation scenario Kinugawa et al 2022), are most likely plunging events.…”

Section: Multi-messenger Signalsmentioning

confidence: 99%

A Channel to Form Fast-spinning Black Hole--Neutron Star Binary Mergers as Multi-messenger Sources

Hu,

Zhu,

Qin

et al. 2022

Preprint

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show abstract

“…The extension of our current grids with many other metallicities (especially lower metallicities) has been considered for our study in the near future. Román-Garza et al (2021) claimed that the fraction of NSfirst-born systems with different SN engines is 10% (see also Kinugawa et al 2022). Recent population synthesis studies Chattopadhyay et al 2021) showed that the fraction of NS-first-born NSBH binaries in total galactic NSBH binaries highly depends on the variations of binary population synthesis assumptions.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…The firstborn BHs in NSBH mergers are expected to have near-zero spin distributions (e.g., Qin et al 2018;Belczynski et al 2020). and Kinugawa et al (2022) suggested that GW200105 and GW200115 are expected to be formed via the classical BH-first-born isolated formation channel. Their posterior distributions of BH projected aligned spin versus BH mass from Abbott et al (2021a) are plotted in Figure 3.…”

Section: Impact Of Sn Kicks On Bh Projected Aligned Spins and The Pro...mentioning

confidence: 99%

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A Channel to Form Fast-spinning Black Hole–Neutron Star Binary Mergers as Multimessenger Sources

Zhu

Qin

et al. 2022

ApJ

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After the successful detection of a gravitational-wave (GW) signal and its associated electromagnetic (EM) counterparts from GW170817, neutron star–black hole (NSBH) mergers have been highly expected to be the next type of multimessenger source. However, despite the detection of several NSBH merger candidates during the GW third observation run, no confirmed EM counterparts from these sources have been identified. The most plausible explanation is that these NSBH merger candidates were plunging events mainly because the primary black holes (BHs) had near-zero projected aligned spins based on GW observations. In view of the fact that neutron stars (NSs) can be easily tidally disrupted by BHs with high projected aligned spins, we study an evolution channel to form NSBH binaries with fast-spinning BHs, the properties of BH mass and spin, and their associated tidal disruption probability. We find that if the NSs are born first, the companion helium stars would be tidally spun up efficiently, and would thus finally form fast-spinning BHs. If BHs do not receive significant natal kicks at birth, these NSBH binaries that can merge within Hubble time would have BHs with projected aligned spins χ z ≳ 0.8 and, hence, can certainly allow tidal disruption to happen. Even if significant BH kicks are considered for a small fraction of NSBH binaries, the projected aligned spins of BHs are χ z ≳ 0.2. These systems can still be disrupted events unless the NSs are very massive. Thus, NS-first-born NSBH mergers would be promising multimessenger sources. We discuss various potential EM counterparts associated with these systems and their detectability in the upcoming fourth observation run.

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Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

2022

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On 11 February 2016, the LIGO and Virgo scientific collaborations announced the first direct detection of gravitational waves, a signal caught by the LIGO interferometers on 14 September 2015, and produced by the coalescence of two stellar-mass black holes. The discovery represented the beginning of an entirely new way to investigate the Universe. The latest gravitational-wave catalog by LIGO, Virgo and KAGRA brings the total number of gravitational-wave events to 90, and the count is expected to significantly increase in the next years, when additional ground-based and space-born interferometers will be operational. From the theoretical point of view, we have only fuzzy ideas about where the detected events came from, and the answers to most of the five Ws and How for the astrophysics of compact binary coalescences are still unknown. In this work, we review our current knowledge and uncertainties on the astrophysical processes behind merging compact-object binaries. Furthermore, we discuss the astrophysical lessons learned through the latest gravitational-wave detections, paying specific attention to the theoretical challenges coming from exceptional events (e.g., GW190521 and GW190814).

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Neutron star black hole binaries in LIGO/Virgo O3b run were formed from Population I/II binaries

Cited by 4 publications

References 33 publications

A Channel to Form Fast-spinning Black Hole--Neutron Star Binary Mergers as Multi-messenger Sources

A Channel to Form Fast-spinning Black Hole--Neutron Star Binary Mergers as Multi-messenger Sources

A Channel to Form Fast-spinning Black Hole–Neutron Star Binary Mergers as Multimessenger Sources

Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

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