Black hole - neutron star mergers: the first mass gap and kilonovae

Drozda, P.; Belczyński, Krzysztof; O’Shaughnessy, R.; Bulik, T.; Fryer, Chris L.

doi:10.48550/arxiv.2009.06655

Cited by 26 publications

(39 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, the predicted brightness for most of kilonovae still be too faint for the follow-up observations of LSST. This result is basically consistent with other recent studies (e.g., Zappa et al 2019;Zhu et al 2020b;Drozda et al 2020). For future GW-triggered multi-messenger observations, one may search for potential sGRB and afterglow as ideal EM counterparts of NSBH GW events.…”

Section: Conclusion and Discussionsupporting

confidence: 92%

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

Zhu

Yang

et al. 2021

ApJ

View full text Add to dashboard Cite

We analyse the tidal disruption probability of potential neutron star-black hole (NSBH) merger gravitational wave (GW) events, including GW190426 152155, GW190814, GW200105 162426 and GW200115 042309, detected during the third observing run of the LIGO/Virgo Collaboration, and the detectability of kilonova emission in connection with these events. The posterior distributions of GW190814 and GW200105 162426 show that they must be plunging events and hence no kilonova signal is expected from these events. With the stiffest NS equation of state allowed by the constraint of GW170817 taken into account, the probability that GW190426 152155 and GW200115 042309 can make tidal disruption is ∼ 24% and ∼ 3%, respectively. However, the predicted kilonova brightness is too faint to be detected for present follow-up search campaigns, which explains the lack of electromagnetic (EM) counterpart detection after triggers of these GW events. Based on the best constrained population synthesis simulation results, we find that disrupted events account for only 20% of cosmological NSBH mergers since most of the primary BHs could have low spins. The associated kilonovae for those disrupted events are still difficult to be discovered by LSST after GW triggers in the future, because of their low brightness and larger distances. For future GW-triggered multi-messenger observations, potential short-duration gamma-ray bursts and afterglows are more probable EM counterparts of NSBH GW events.

show abstract

Section: Conclusion and Discussionsupporting

confidence: 92%

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

Zhu

Yang

et al. 2021

ApJ

View full text Add to dashboard Cite

show abstract

“…The survey projects we consider in this work include the Zwicky Transient Facility (ZTF; Bellm et al 2019;Masci et al 2019), the Multichannel Photometric Survey Telescope 2 (Mephisto; Er et al 2021, in preparation), the Wide Field Survey Telescope (WFST;et al Kong et al 2021, in preparation), the Large Synoptic Survey Telescope (LSST; LSST Science Collaboration et al 2009), and the SiTian Projects (SiTian; Liu et al 2021). We note that NSBH mergers may have a lower event rate density, that NSBH kilonovae may be dimmer than BNS kilonovae (e.g., Zhu et al 2020) and that most NSBH mergers in the universe are likely plunging events (e.g., Abbott et al 2021a;Zappa et al 2019;Drozda et al 2020;Zhu et al 2021c;Broekgaarden et al 2021). As a result, the detection rates of kilonova and afterglow emissions from NSBH mergers should be much lower than those from BNS mergers (Zhu et al 2021f).…”

Section: Introductionmentioning

confidence: 73%

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Zhu¹,

Wu²,

Yang³

et al. 2021

Preprint

View full text Add to dashboard Cite

In the second work of this series, we explore the optimal search strategy for serendipitous and gravitational-wave-triggered target-of-opportunity observations of kilonovae and optical short-duration gamma-ray burst (sGRB) afterglows from binary neutron star (BNS) mergers, assuming that cosmological kilonovae are AT2017gfo-like (but with viewing-angle dependence) and that the properties of afterglows are consistent with those of cosmological sGRB afterglows. A one-day cadence serendipitous search strategy with an exposure time of ∼ 30 s can always achieve an optimal search strategy of kilonovae and afterglows for various survey projects. We show that the optimal detection rates of the kilonova-dominated (afterglow-dominated) events are ∼ 0.2/0.5/0.8/20 yr −1 (∼ 500/300/600/3000 yr −1 ) for ZTF/Mephisto/WFST/LSST, respectively. A better search strategy for SiTian is to increase the exposure time. SiTian can find ∼ 5(6000) yr −1 kilonova-dominated (afterglow-dominated) events. We predict abundant off-axis orphan afterglows may be recorded in the survey database although not been identified. For target-of-opportunity observations, we simulate the maximum BNS gravitational-wave (GW) detection rates, which are ∼ 27/210/1800/2.0 × 10 5 yr −1 , in the networks of 2nd/2.5th/3rd(Voyager)/3rd(ET&CE)-generation GW detectors. In the upcoming 2nd-generation networks, follow-up observations with a limiting magnitude of m limit 22 − 23 mag can discover all EM signals from BNS GW events. Among these detected GW events, ∼ 60% events (∼ 16 yr −1 ) can detect clear kilonova signals, while afterglow-dominated events would account for the other ∼ 40% events (∼ 11 yr −1 ). In the 2.5th-and 3rd(Voyager)-generation era, the critical magnitudes for the detection of EM emissions from all BNS GW events would be ∼ 23.5 mag and ∼ 25 mag, respectively. Foreseeable optical survey projects cannot detect all EM signals of GW events detected during the ET&CE era.

show abstract

“…The most widely accepted formation channel for the majority of NSBH binaries in the universe is the classical Common Envelope (CE) scenario (e.g., Giacobbo & Mapelli 2018;Belczynski et al 2020;Drozda et al 2020;Shao & Li 2021;. In this scenario, the immediate progenitor of a NSBH binary just after the CE phase is a close binary system, which consists of a compact object (NS or BH) and a helium star.…”

Section: Introductionmentioning

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

View full text Add to dashboard Cite

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.

show abstract

Black hole - neutron star mergers: the first mass gap and kilonovae

Cited by 26 publications

References 72 publications

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

No Detectable Kilonova Counterpart is Expected for O3 Neutron Star–Black Hole Candidates

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

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

Contact Info

Product

Resources

About