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A Triple Scenario for the Formation of Wide Black Hole Binaries Such As Gaia BH1
Solar and Stellar Astrophysics · Submitted 5 Dec 2023
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Here we show that such systems can indeed be more easily explained via evolution in hierarchical triple systems. von Zeipel-Lidov-Kozai oscillations or instabilities can delay the onset of the common envelope phase in the inner binary of the triple, so that the black hole progenitor and low-mass star are more widely separated when it begins, leading to the formation of wider binaries.
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The abstract, sentence by sentence
Recently, several non-interacting black hole-stellar binaries have been identified in Gaia data. For example, Gaia BH1, where a Sun-like star is in a moderate eccentricity (e=0.44), 185-day orbit around a black hole. This orbit is difficult to explain through binary evolution. The present-day separation suggests the progenitor system would have undergone an episode of common envelope evolution, but a common envelope should shrink the period below the observed one. Since the majority of massive stars form in higher multiplicity systems, a triple evolution scenario is more likely for the progenitors of BH binaries. Here we show that such systems can indeed be more easily explained via evolution in hierarchical triple systems. von Zeipel-Lidov-Kozai oscillations or instabilities can delay the onset of the common envelope phase in the inner binary of the triple, so that the black hole progenitor and low-mass star are more widely separated when it begins, leading to the formation of wider binaries. There are also systems with similar periods but larger eccentricities, where the BH progenitor is a merger product of the inner binary in the triple. Such mergers lead to a more top-heavy black hole mass function.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Recently, several non-interacting black hole-stellar binaries have been identified in Gaia data. | background 1.00 | 0.06 | 0.02 | asserted 1.00 |
| s1 | For example, Gaia BH1, where a Sun-like star is in a moderate eccentricity (e=0.44), 185-day orbit around a black hole. | background 0.99 | 0.09 | 0.02 | asserted 1.00 |
| s2 | This orbit is difficult to explain through binary evolution. | background 0.51 | 0.14 | 0.03 | asserted 0.96 |
| s3 | The present-day separation suggests the progenitor system would have undergone an episode of common envelope evolution, but a common envelope should shrink the period below the observed one. | background 0.55 | 0.16 | 0.03 | hedged possibility 0.72 |
| s4 | Since the majority of massive stars form in higher multiplicity systems, a triple evolution scenario is more likely for the progenitors of BH binaries. | background 0.90 | 0.09 | 0.12 | hedged possibility 0.98 |
| s5 | Here we show that such systems can indeed be more easily explained via evolution in hierarchical triple systems. von Zeipel-Lidov-Kozai oscillations or instabilities can delay the onset of the common envelope phase in the inner binary of the triple, so that the black hole progenitor and low-mass star are more widely separated when it begins, leading to the formation of wider binaries. | contribution 0.92 | 0.81 | 0.90 | asserted 0.95 |
| s6 | There are also systems with similar periods but larger eccentricities, where the BH progenitor is a merger product of the inner binary in the triple. | result 0.81 | 0.41 | 0.06 | asserted 0.97 |
| s7 | Such mergers lead to a more top-heavy black hole mass function. | interpretation 0.76 | 0.41 | 0.07 | asserted 1.00 |
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Original abstract
Recently, several non-interacting black hole-stellar binaries have been identified in Gaia data. For example, Gaia BH1, where a Sun-like star is in a moderate eccentricity (e=0.44), 185-day orbit around a black hole. This orbit is difficult to explain through binary evolution. The present-day separation suggests the progenitor system would have undergone an episode of common envelope evolution, but a common envelope should shrink the period below the observed one. Since the majority of massive stars form in higher multiplicity systems, a triple evolution scenario is more likely for the progenitors of BH binaries. Here we show that such systems can indeed be more easily explained via evolution in hierarchical triple systems. von Zeipel-Lidov-Kozai oscillations or instabilities can delay the onset of the common envelope phase in the inner binary of the triple, so that the black hole progenitor and low-mass star are more widely separated when it begins, leading to the formation of wider binaries. There are also systems with similar periods but larger eccentricities, where the BH progenitor is a merger product of the inner binary in the triple. Such mergers lead to a more top-heavy black hole mass function.
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References
How the literature uses it
4 arXiv papers cite this in 4 sentences
What it cites · 3 sentences without a confident label
Uses data or values from 1 paper
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Previously, [ref] find a total of $4.2 ×10^-7$ ($1.2×10^-5$) BH-MS binaries (with periods up to 10 yr[Wider systems would not be detectable by Gaia.]) per unit star formation from isolated binary evolution (open clusters).
Young Star Clusters Dominate the Production of Detached Black Hole-Star Binaries · Rates · 0.88
Cites as background 1 paper
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Previous work has estimated the formation rate of BH-main sequence binaries in open star clusters [ref] .
Young Star Clusters Dominate the Production of Detached Black Hole-Star Binaries · Rates · 0.90
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