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

Hu, Rui-Chong; Zhu, Jin-Ping; Qin, Ying; Zhang, Bing; Liang, En-Wei; Shao, Yong

doi:10.48550/arxiv.2201.09549

Cited by 3 publications

(3 citation statements)

References 48 publications

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“…Mandel and Smith [582] reanalyzed the GW200115 signal using astrophysically-motivated spin priors and they obtained better constrains on the masses of the compact objects (m 1 = 7.0 +0.4 −0.4 M , m 2 = 1.25 +0.09 −0.07 M ) and a BH spin close to zero (χ 1,z = 0.00 +0.04 −0.04 ). The spins of the secondaries are unconstrained and no electromagnetic counterpart has been identified for both the events, in agreement with theoretical expectations for mixed binaries with low-spinning primary BHs (e.g., [583,584], but see [585]).…”

Section: Gw200105_162426 and Gw200115_042309supporting

confidence: 83%

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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Section: Gw200105_162426 and Gw200115_042309supporting

confidence: 83%

Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

2022

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“…"Pessimistic" is our base model, with one key assumption about binary or stellar evolution varied in each of the following three models. In our 2 NSBH systems are exciting especially as multi-messenger sources -they can harbour recycled pulsars (Chattopadhyay et al 2021) as the NSs is born first and NSBHs with high pre-merger BH spins have the possibility to produce exciting electromagnetic signatures at their mergers (Hu et al 2022) choice of parameters for the models, we are guided by Fiducial/Default models of previous population synthesis studies (Stevenson et al 2017;Vigna-Gómez et al 2018;Neijssel et al 2019;Chattopadhyay et al 2020Chattopadhyay et al , 2021Broekgaarden et al 2021a). Based on the recent results from Broekgaarden & Berger (2021), we place particular emphasis on the importance of neutron star natal kicks, and the efficiency of the common envelope phase of binary evolution.…”

Section: Methodsmentioning

confidence: 99%

Modelling the formation of the first two neutron star-black hole mergers, GW200105 and GW200115: metallicity, chirp masses and merger remnant spins

Chattopadhyay,

Stevenson,

Broekgaarden

et al. 2022

Preprint

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The two neutron star-black hole mergers (GW200105 and GW200115) observed in gravitational waves by advanced LIGO and Virgo, mark the first ever discovery of such binaries in nature. We study these two neutron star-black hole systems through isolated binary evolution, using a grid of population synthesis models. Using both mass and spin observations (chirp mass, effective spin and remnant spin) of the binaries, we probe their different possible formation channels in different metallicity environments. Our models only support LIGO data when assuming the black hole is non spinning. Our results show a strong preference that GW200105 and GW200115 formed from stars with sub-solar metallicities 𝑍 0.005. Only two metal-rich (𝑍 = 0.02) models are in agreement with GW200115. We also find that chirp mass and remnant spins jointly aid in constraining the models, whilst the effective spin parameter does not add any further information.

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“…In Pathway A2, tides can affect both WR stars potentially allowing for a high BH spin, but this requires fine-tuning to ensure that the secondary is still not too massive to form a BH, e.g., qZAMS ∼ 0.95. If tidal interactions were to produce a highly spinning and aligned WR star such a system may yield significant ejected mass (Hu et al 2022).…”

Section: Black-hole Neutron-star Binary Formationmentioning

confidence: 99%

Mechanisms for high spin in black-hole neutron-star binaries and kilonova emission: inheritance and accretion

Steinle¹,

Gompertz²,

Nicholl³

2022

Preprint

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Black-hole neutron-star binary mergers, whose existence has been confirmed by gravitational-wave detectors, can lead to an electromagnetic counterpart called a kilonova if the neutron star is disrupted prior to merger. The observability of a kilonova depends crucially on the amount of neutron star ejecta, which is sensitive to the aligned component of the black hole spin. These binaries likely originate from the evolution of isolated stellar binaries. We explore the dependence of the ejected mass on two main mechanisms that provide high black hole spin. When the black hole inherits a high spin from a Wolf-Rayet star that was born with least ∼ 10% of its breakup spin under weak stellar core-envelope coupling, which is relevant for all formation pathways, the median of the ejected mass is 10 −2 M . Though only possible for certain formation pathways, similarly large ejected mass results when the BH accretes 20% of its companion's envelope to gain a high spin, and a more massive stellar progenitor provides smaller ejected mass compared to when the black hole inherits high spin. Together, these signatures suggest that a population analysis of black hole masses and spins in black-hole neutron-star binary mergers may help distinguish between mechanisms for spin and possible formation pathways. Using a novel kilonova light curve model we show that current capabilities are unlikely to observe a counterpart, however future facilities such as the Vera Rubin Observatory will likely detect counterparts even if the aligned dimensionless spin of the disrupting black hole is as low as ∼ 0.2. Our model predicts kilonovae as bright as M i ∼ −14.5 for an aligned black hole spin of ∼ 0.9.

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

Cited by 3 publications

References 48 publications

Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

Compact Binary Coalescences: Astrophysical Processes and Lessons Learned

Modelling the formation of the first two neutron star-black hole mergers, GW200105 and GW200115: metallicity, chirp masses and merger remnant spins

Mechanisms for high spin in black-hole neutron-star binaries and kilonova emission: inheritance and accretion

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