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Binaries migrating in a gaseous disk: Where are the Galactic center binaries?

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C. Baruteau, J. Cuadra, D. N. C. Lin

Astrophysics of Galaxies · Submitted 1 Nov 2010

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

The authors' main claim Such processes may provide an alternative unified scenario for the origin of the kinematic properties of the central cluster and S-stars in the Galactic center as well as the high velocity stars in the Galactic halo.

how it is stated · hedged possibility 1.00 read the record →

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arXiv ID1011.0360 (version 1)
Pith IDHNVJAZZ2, Pith's permanent record of this paper and its review
CitationC. Baruteau, D. N. C. Lin, J. Cuadra. "Binaries migrating in a gaseous disk: Where are the Galactic center binaries?." arXiv:1011.0360 (2010). https://pith.science/paper/HNVJAZZ2
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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, 8,221 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.16 · human participants 0.01 · controlled comparison 0.30 · randomized assignment 0.01 · states quantitative result 0.12 · compares with prior results 0.28 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

The massive stars in the Galactic center inner arcsecond share analogous properties with the so-called Hot Jupiters. Most of these young stars have highly eccentric orbits, and were probably not formed in-situ. It has been proposed that these stars acquired their current orbits from the tidal disruption of compact massive binaries scattered toward the proximity of the central supermassive black hole. Assuming a binary star formed in a thin gaseous disk beyond 0.1 pc from the central object, we investigate the relevance of disk-satellite interactions to harden the binding energy of the binary, and to drive its inward migration. A massive, equal-mass binary star is found to become more tightly wound as it migrates inwards toward the central black hole. The migration timescale is very similar to that of a single-star satellite of the same mass. The binary's hardening is caused by the formation of spiral tails lagging the stars inside the binary's Hill radius. We show that the hardening timescale is mostly determined by the mass of gas inside the binary's Hill radius, and that it is much shorter than the migration timescale. We discuss some implications of the binary's hardening process. When the more massive (primary) components of close binaries eject most their mass through supernova explosion, their secondary stars may attain a range of eccentricities and inclinations. Such processes may provide an alternative unified scenario for the origin of the kinematic properties of the central cluster and S-stars in the Galactic center as well as the high velocity stars in the Galactic halo.

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 The massive stars in the Galactic center inner arcsecond share analogous properties with the so-called Hot Jupiters. background 0.99 0.18 0.03 asserted 1.00
s1 Most of these young stars have highly eccentric orbits, and were probably not formed in-situ. background 1.00 0.14 0.03 hedged possibility 0.74
s2 It has been proposed that these stars acquired their current orbits from the tidal disruption of compact massive binaries scattered toward the proximity of the central supermassive black hole. background 1.00 0.03 0.05 hedged possibility 0.74
s3 Assuming a binary star formed in a thin gaseous disk beyond 0.1 pc from the central object, we investigate the relevance of disk-satellite interactions to harden the binding energy of the binary, and to drive its inward migration. contribution 0.87 0.59 0.05 asserted 0.31
s4 A massive, equal-mass binary star is found to become more tightly wound as it migrates inwards toward the central black hole. result 1.00 0.91 0.26 asserted 1.00
s5 The migration timescale is very similar to that of a single-star satellite of the same mass. result 1.00 0.80 0.11 asserted 1.00
s6 The binary's hardening is caused by the formation of spiral tails lagging the stars inside the binary's Hill radius. result 0.75 0.83 0.15 asserted 1.00
s7 We show that the hardening timescale is mostly determined by the mass of gas inside the binary's Hill radius, and that it is much shorter than the migration timescale. result 0.98 0.92 0.31 asserted 1.00
s8 We discuss some implications of the binary's hardening process. interpretation 0.85 0.38 0.03 unclear 0.97
s9 When the more massive (primary) components of close binaries eject most their mass through supernova explosion, their secondary stars may attain a range of eccentricities and inclinations. interpretation 0.84 0.11 0.08 hedged possibility 1.00
s10 Such processes may provide an alternative unified scenario for the origin of the kinematic properties of the central cluster and S-stars in the Galactic center as well as the high velocity stars in the Galactic halo. interpretation 1.00 0.15 0.32 hedged possibility 1.00

What kind of paper the classifier reports this is: simulation study 0.98 · evidence from simulation or computation 0.99.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
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

The massive stars in the Galactic center inner arcsecond share analogous properties with the so-called Hot Jupiters. Most of these young stars have highly eccentric orbits, and were probably not formed in-situ. It has been proposed that these stars acquired their current orbits from the tidal disruption of compact massive binaries scattered toward the proximity of the central supermassive black hole. Assuming a binary star formed in a thin gaseous disk beyond 0.1 pc from the central object, we investigate the relevance of disk-satellite interactions to harden the binding energy of the binary, and to drive its inward migration. A massive, equal-mass binary star is found to become more tightly wound as it migrates inwards toward the central black hole. The migration timescale is very similar to that of a single-star satellite of the same mass. The binary's hardening is caused by the formation of spiral tails lagging the stars inside the binary's Hill radius. We show that the hardening timescale is mostly determined by the mass of gas inside the binary's Hill radius, and that it is much shorter than the migration timescale. We discuss some implications of the binary's hardening process. When the more massive (primary) components of close binaries eject most their mass through supernova explosion, their secondary stars may attain a range of eccentricities and inclinations. Such processes may provide an alternative unified scenario for the origin of the kinematic properties of the central cluster and S-stars in the Galactic center as well as the high velocity stars in the Galactic halo.

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References
How later papers used it

68 later papers cite it

Evidence: substantial. 63 of the citing papers share no author with it, and 10 of those carry a confident label from Pith's citation classifier.

Pith read 13 of the 107 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Uses its method or tool 2 papers
Uses its data or values 1 of 4 papers with this label
How the literature uses it

5 arXiv papers cite this in 7 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 6 sentences without a confident label

Uses its data or values 1 paper
  • Using the standard $α$-prescription for local turbulent viscosity in AGN disks, the migration timescales for single stars/BHs are estimated to be, $τ_Type I ∼10^7$ years and $τ_Type II ∼10^8$ years [ref] .

    Blackhole Mergers Through Evection Resonances · Disk Migration · 0.94

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