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The Role of Chaos in the Circularization of Tidal Capture Binaries. II. Long-Term Evolution
Astrophysics · Submitted 22 Dec 1993
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim If dissipation is taken into account, the binary goes through a short and violent chaotic phase, followed by a long quiescent phase in which it slowly circularizes from a high eccentricity on a much longer timescale than previously thought.
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A self-consistent, adiabatic model for the {\it long-time} behaviour of tidal capture binaries is presented. It is shown that most capture orbits behave chaotically, with the eccentricity following a quasi-random walk between the values of $\appless 1$ and some lower limit associated with the periastron separation at capture. If dissipation is taken into account, the binary goes through a short and violent chaotic phase, followed by a long quiescent phase in which it slowly circularizes from a high eccentricity on a much longer timescale than previously thought. A consequence is that merger is less likely than previously thought, and hence such binaries will be available as a heat source to the cores of globular clusters, particularly while they are in the less tightly bound, highly eccentric phase. If the model is correct, any highly eccentric binaries observed in globular clusters which contain a main-sequence star will most likely be found to have a period derivative much smaller than that predicted by the standard model. We also predict that the companion of PSR B1718-19 in NGC 6342 which is a globular cluster binary likely to have been formed by tidal capture (Wijers \& Paczy\'{n}ski 1993) will be found to have a mass of around $0.2M_\odot$. The model may be used to describe the evolution of low-mass X-ray binaries, pulsar binaries, and cataclysmic binaries which abound in globular clusters.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | A self-consistent, adiabatic model for the {\it long-time} behaviour of tidal capture binaries is presented. | contribution 0.69 | 0.90 | 0.07 | asserted 0.98 |
| s1 | It is shown that most capture orbits behave chaotically, with the eccentricity following a quasi-random walk between the values of $\appless 1$ and some lower limit associated with the periastron separation at capture. | result 1.00 | 0.85 | 0.19 | asserted 1.00 |
| s2 | If dissipation is taken into account, the binary goes through a short and violent chaotic phase, followed by a long quiescent phase in which it slowly circularizes from a high eccentricity on a much longer timescale than previously thought. | result 1.00 | 0.82 | 0.48 | asserted 0.88 |
| s3 | A consequence is that merger is less likely than previously thought, and hence such binaries will be available as a heat source to the cores of globular clusters, particularly while they are in the less tightly bound, highly eccentric phase. | interpretation 0.99 | 0.68 | 0.28 | asserted 0.90 |
| s4 | If the model is correct, any highly eccentric binaries observed in globular clusters which contain a main-sequence star will most likely be found to have a period derivative much smaller than that predicted by the standard model. | interpretation 0.72 | 0.54 | 0.14 | hedged possibility 0.94 |
| s5 | We also predict that the companion of PSR B1718-19 in NGC 6342 which is a globular cluster binary likely to have been formed by tidal capture (Wijers \& Paczy\'{n}ski 1993) will be found to have a mass of around $0.2M_\odot$. | result 0.81 | 0.66 | 0.04 | hedged possibility 0.44 |
| s6 | The model may be used to describe the evolution of low-mass X-ray binaries, pulsar binaries, and cataclysmic binaries which abound in globular clusters. | interpretation 0.55 | 0.42 | 0.05 | hedged possibility 1.00 |
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Original abstract
A self-consistent, adiabatic model for the {\it long-time} behaviour of tidal capture binaries is presented. It is shown that most capture orbits behave chaotically, with the eccentricity following a quasi-random walk between the values of $\appless 1$ and some lower limit associated with the periastron separation at capture. If dissipation is taken into account, the binary goes through a short and violent chaotic phase, followed by a long quiescent phase in which it slowly circularizes from a high eccentricity on a much longer timescale than previously thought. A consequence is that merger is less likely than previously thought, and hence such binaries will be available as a heat source to the cores of globular clusters, particularly while they are in the less tightly bound, highly eccentric phase. If the model is correct, any highly eccentric binaries observed in globular clusters which contain a main-sequence star will most likely be found to have a period derivative much smaller than that predicted by the standard model. We also predict that the companion of PSR B1718-19 in NGC 6342 which is a globular cluster binary likely to have been formed by tidal capture (Wijers \& Paczy\'{n}ski 1993) will be found to have a mass of around $0.2M_\odot$. The model may be used to describe the evolution of low-mass X-ray binaries, pulsar binaries, and cataclysmic binaries which abound in globular clusters.
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