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Successive Merger of Multiple Massive Black Holes in a Primordial Galaxy

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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Ataru Tanikawa, Masayuki Umemura

Astrophysics of Galaxies · Submitted 12 Jan 2011

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The simulations show that a multiple MBH system can produce a heavier MBH at the galactic center purely through $N$-body process.

how it is stated · asserted 0.99 read the record →

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arXiv ID1101.2263 (version 2)
Pith IDXXHX2RFB, Pith's permanent record of this paper and its review
CitationAtaru Tanikawa, Masayuki Umemura. "Successive Merger of Multiple Massive Black Holes in a Primordial Galaxy." arXiv:1101.2263 (2011). https://pith.science/paper/XXHX2RFB
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The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 8,278 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.71 · human participants 0.01 · controlled comparison 0.02 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.10 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

Using highly-accurate $N$-body simulations, we explore the evolution of multiple massive black holes (hereafter, MBHs) in a primordial galaxy that is composed of stars and MBHs. The evolution is pursed with a fourth-order Hermite scheme, where not only three-body interaction of MBHs but also dynamical friction by stars are incorporated. Initially, ten MBHs with equal mass of $10^7M_\odot$ are set in a host galaxy with $10^{11}M_\odot$. It is found that 4 - 6 MBHs merge successively within 1 Gyr, emitting gravitational wave radiation. The key process for the successive merger of MBHs is the dynamical friction by field stars, which enhances three-body interactions of MBHs when they enter the central regions of the galaxy. The heaviest MBH always composes a close binary at the galactic center, which shrinks owing to the angular momentum transfer by the third MBH and eventually merges. The angular momentum transfer by the third MBH is due to the sling-shot mechanism. We find that the secular Kozai mechanism does not work for a binary to merge if we include the relativistic pericenter shift. The simulations show that a multiple MBH system can produce a heavier MBH at the galactic center purely through $N$-body process. This merger path can be of great significance for the growth of MBHs in a primordial galaxy. The merger of multiple MBHs may be a potential source of gravitational waves for the Laser Interferometer Space Antenna (LISA) and pulsar timing.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Using highly-accurate $N$-body simulations, we explore the evolution of multiple massive black holes (hereafter, MBHs) in a primordial galaxy that is composed of stars and MBHs. contribution 0.88 0.92 0.03 asserted 0.68
s1 The evolution is pursed with a fourth-order Hermite scheme, where not only three-body interaction of MBHs but also dynamical friction by stars are incorporated. method 1.00 0.83 0.03 asserted 0.99
s2 Initially, ten MBHs with equal mass of $10^7M_\odot$ are set in a host galaxy with $10^{11}M_\odot$. method 0.97 0.82 0.03 asserted 0.98
s3 It is found that 4 - 6 MBHs merge successively within 1 Gyr, emitting gravitational wave radiation. result 1.00 0.96 0.38 asserted 1.00
s4 The key process for the successive merger of MBHs is the dynamical friction by field stars, which enhances three-body interactions of MBHs when they enter the central regions of the galaxy. interpretation 0.85 0.91 0.27 asserted 1.00
s5 The heaviest MBH always composes a close binary at the galactic center, which shrinks owing to the angular momentum transfer by the third MBH and eventually merges. result 0.94 0.91 0.14 asserted 1.00
s6 The angular momentum transfer by the third MBH is due to the sling-shot mechanism. interpretation 0.83 0.61 0.05 asserted 1.00
s7 We find that the secular Kozai mechanism does not work for a binary to merge if we include the relativistic pericenter shift. result 0.99 0.94 0.06 asserted 1.00
s8 The simulations show that a multiple MBH system can produce a heavier MBH at the galactic center purely through $N$-body process. result 0.94 0.95 0.59 asserted 0.99
s9 This merger path can be of great significance for the growth of MBHs in a primordial galaxy. interpretation 1.00 0.41 0.21 hedged possibility 0.78
s10 The merger of multiple MBHs may be a potential source of gravitational waves for the Laser Interferometer Space Antenna (LISA) and pulsar timing. interpretation 0.99 0.49 0.09 hedged possibility 1.00

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

Using highly-accurate $N$-body simulations, we explore the evolution of multiple massive black holes (hereafter, MBHs) in a primordial galaxy that is composed of stars and MBHs. The evolution is pursed with a fourth-order Hermite scheme, where not only three-body interaction of MBHs but also dynamical friction by stars are incorporated. Initially, ten MBHs with equal mass of $10^7M_\odot$ are set in a host galaxy with $10^{11}M_\odot$. It is found that 4 - 6 MBHs merge successively within 1 Gyr, emitting gravitational wave radiation. The key process for the successive merger of MBHs is the dynamical friction by field stars, which enhances three-body interactions of MBHs when they enter the central regions of the galaxy. The heaviest MBH always composes a close binary at the galactic center, which shrinks owing to the angular momentum transfer by the third MBH and eventually merges. The angular momentum transfer by the third MBH is due to the sling-shot mechanism. We find that the secular Kozai mechanism does not work for a binary to merge if we include the relativistic pericenter shift. The simulations show that a multiple MBH system can produce a heavier MBH at the galactic center purely through $N$-body process. This merger path can be of great significance for the growth of MBHs in a primordial galaxy. The merger of multiple MBHs may be a potential source of gravitational waves for the Laser Interferometer Space Antenna (LISA) and pulsar timing.

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