Formation and Merging of Mass Gap Black Holes in Gravitational-wave Merger Events from Wide Hierarchical Quadruple Systems

Safarzadeh, Mohammadtaher; Hamers, Adrian S.; Loeb, Abraham; Berger, E.

doi:10.3847/2041-8213/ab5dc8

Cited by 59 publications

(36 citation statements)

References 52 publications

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“…BBHs in triple or quadruple systems can undergo Lidov-Kozai oscillations [211,212] that may expedite the GW inspiral of the binary. Such systems can either exist in the galactic field with a stellar-mass outer perturber [213][214][215][216][217][218][219] or in galactic nuclei with a supermassive BH as the tertiary component [220][221][222][223]. Though most modeling of hierarchical stellar systems does not include robust predictions for mass ratio distributions of merging BBHs, certain models find galactic field triples with asymmetric masses for the inner BBH to have a merger fraction that is about twice as large as their equalmass counterparts [213].…”

Section: Astrophysical Formation Channels For Gw190412mentioning

confidence: 99%

GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Abbott¹,

Abbott²,

Abraham³

et al. 2020

Phys. Rev. D

557

408

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We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO's and Virgo's third observing run. The signal was recorded on April 12, 2019 at 05∶30∶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ∼30 M ⊙ black hole merged with a ∼8 M ⊙ black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein's general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs.

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Section: Astrophysical Formation Channels For Gw190412mentioning

confidence: 99%

GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Abbott¹,

Abbott²,

Abraham³

et al. 2020

Phys. Rev. D

557

408

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“…Secular perturbation by the supermassive BH's tidal field may subsequently excite large eccentricity in the remnant bBH system and lead to merger, but most likely at a very low rate (Fragione, Leigh & Perna 2019). Another possibility is to invoke an additional body in a hierarchical quadruple system in the field, with either '2 + 2' or '3 + 1' configuration such that after the bNS merger, the remaining three bodies undergo chaotic evolution to generate the second-generation merger, but such finetuned situation may occur at a very low rate (Fragione, Loeb & Rasio 2020;Liu & Lai 2020;Safarzadeh et al 2020).…”

mentioning

confidence: 99%

On the formation of GW190814

Beniamini

Bonnerot

2020

Monthly Notices of the Royal Astronomical Society

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The LIGO-Virgo collaboration recently reported a puzzling event, GW190814, with component masses of 23 and 2.6M⊙. Motivated by the relatively small rate of such a coalescence (1–$23\rm \, Gpc^{-3}\, yr^{-1}$) and the fact that the mass of the secondary is close to the total mass of known binary neutron star (bNS) systems, we propose that GW190814 was a second-generation merger from a hierarchical triple system, i.e. the remnant from the bNS coalescence was able to merge again with the 23M⊙ black hole (BH) tertiary. We show that this occurs at a sufficiently high probability provided that the semimajor axis of the outer orbit is less than a few AU at the time of bNS coalescence. It remains to be explored whether the conditions for the formation of such tight triple systems are commonly realized in the Universe, especially in low metallicity (≲ 0.1Z⊙) environments. Our model provides a number of predictions. (1) The spin of the secondary in GW190814-like systems is 0.6–0.7. (2) The component mass distribution from a large sample of LIGO sources should have a narrow peak between 2.5 and ∼3.5M⊙, whereas the range between ∼3.5 and ∼5M⊙ stays empty (provided that stellar evolution does not generate such BHs in the ‘mass gap’). (3) About 90 per cent (10 per cent) of GW190814-like events have an eccentricity of e ≳ 2 × 10−3 (≳ 0.1) near gravitational wave frequency of 10 mHz. (4) A significant fraction ($\gtrsim 10{{\ \rm per\ cent}}$) of bNS mergers should have signatures of a massive tertiary at a distance of a few AU in the gravitational waveform. (5) There are 105 undetected radio-quiet bNS systems with a massive BH tertiary in the Milky Way.

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“…The observational missing of the intermediate mass black holes is the challenging topic which needs to be solved experimentally and theoretically. The dark stars with Planck core [8], BH-NS mergers [9], merging neutron stars [10,11], supermassive black hole at Milky way galaxy [12], binary BH mergers [13,14], BH mass gap [15] and supermassive black hole masses [16] are some of the interesting research subjects.…”

Section: Introductionmentioning

confidence: 99%

Origins of Stellar Mass Neutron Black Holes, Supermassive Dark Matter Black Holes and Universe Evolution

Hwang¹

2021

Preprint

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The origins of the stellar mass neutron black holes and supermassive dark matter black holes without the singularities are reported based on the 4-D Euclidean space. The neutron black holes with the mass of mBH = 5 – 15 msun are made by the 6-quark merged states (N6q) of two neutrons with the mass (m(N6q) = 10 m(n)) of 9.4 GeV/c2 that gives the black hole mass gap of mBH = 3 – 5 msun. Also, the supermassive black holes with the mass of mSMBH = 106 – 1011 msun are made by the merged 3-D states (J(B1B2B3)3 particles) of the dark matters. The supermassive black hole at the center of the Milky way galaxy has the mass of mSMBH = 4.1 106 msun that is consistent with mSMBH = 2.08 - 6.23 106 msun calculated from the 3-D states (J(B1B2B3)3 particles) of the dark matters with the mass of m(J) = 1.95 1015 eV/c2. In other words, this supports the existence of the B1, B2 and B3 dark matters with the proposed masses. The first dark matter black hole (primary black hole) was created at the big bang. This first dark matter black hole decayed to the supermassive dark matter black holes through the secondary dark matter black holes that are explained by the merged states of the J(B1B2B3)3 particles. The universe evolution is closely connected to the decaying process of the dark matter black holes since the big bang. The dark matter cloud states are proposed at the intermediate mass black hole range of mIMBH = 102 – 105 msun. This can explain why the dark matter black holes are not observed at the intermediate mass black hole range of mIMBH = 102 – 105 msun.

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Formation and Merging of Mass Gap Black Holes in Gravitational-wave Merger Events from Wide Hierarchical Quadruple Systems

Cited by 59 publications

References 52 publications

GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

On the formation of GW190814

Origins of Stellar Mass Neutron Black Holes, Supermassive Dark Matter Black Holes and Universe Evolution

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