Innermost Stable Circular Orbit of Inspiraling Neutron-Star Binaries: Tidal Effects, Post-Newtonian Effects and the Neutron-Star Equation of State

Alan G. Wiseman (Caltech); Dong Lai

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Innermost Stable Circular Orbit of Inspiraling Neutron-Star Binaries: Tidal Effects, Post-Newtonian Effects and the Neutron-Star Equation of State

Dong Lai, Alan G. Wiseman (Caltech)

General Relativity and Quantum Cosmology · Submitted 5 Sep 1996

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

The authors' main claim This suggests that information about the equation of state of nuclear matter is encoded in the gravitational waves emitted just prior to the merger.

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

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arXiv IDgr-qc/9609014 (version 1)

Pith IDJCPCIQ2M, Pith's permanent record of this paper and its review

CitationAlan G. Wiseman (Caltech), Dong Lai. "Innermost Stable Circular Orbit of Inspiraling Neutron-Star Binaries: Tidal Effects, Post-Newtonian Effects and the Neutron-Star Equation of State." arXiv:gr-qc/9609014 (1996). https://pith.science/paper/JCPCIQ2M

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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, 3,788 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.15 · human participants 0.01 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.94 · compares with prior results 0.06 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

We study how the neutron-star equation of state affects the onset of the dynamical instability in the equations of motion for inspiraling neutron-star binaries near coalescence. A combination of relativistic effects and Newtonian tidal effects cause the stars to begin their final, rapid, and dynamically-unstable plunge to merger when the stars are still well separated and the orbital frequency is $\approx$ 500 cycles/sec (i.e. the gravitational wave frequency is approximately 1000 Hz). The orbital frequency at which the dynamical instability occurs (i.e. the orbital frequency at the innermost stable circular orbit) shows modest sensitivity to the neutron-star equation of state (particularly the mass-radius ratio, $M/R_o$, of the stars). This suggests that information about the equation of state of nuclear matter is encoded in the gravitational waves emitted just prior to the merger.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We study how the neutron-star equation of state affects the onset of the dynamical instability in the equations of motion for inspiraling neutron-star binaries near coalescence.	contribution 1.00	0.86	0.07	asserted 0.52
s1	A combination of relativistic effects and Newtonian tidal effects cause the stars to begin their final, rapid, and dynamically-unstable plunge to merger when the stars are still well separated and the orbital frequency is $\approx$ 500 cycles/sec (i.e. the gravitational wave frequency is approximately 1000 Hz).	result 1.00	0.75	0.23	asserted 1.00
s2	The orbital frequency at which the dynamical instability occurs (i.e. the orbital frequency at the innermost stable circular orbit) shows modest sensitivity to the neutron-star equation of state (particularly the mass-radius ratio, $M/R_o$, of the stars).	result 1.00	0.85	0.29	asserted 0.99
s3	This suggests that information about the equation of state of nuclear matter is encoded in the gravitational waves emitted just prior to the merger.	interpretation 1.00	0.46	0.66	hedged possibility 1.00

What kind of paper the classifier reports this is: theoretical result 0.71 · evidence from simulation or computation 0.64.

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arXiv listing abstract v1

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full text
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references and citing sentences
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S sections
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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

We study how the neutron-star equation of state affects the onset of the dynamical instability in the equations of motion for inspiraling neutron-star binaries near coalescence. A combination of relativistic effects and Newtonian tidal effects cause the stars to begin their final, rapid, and dynamically-unstable plunge to merger when the stars are still well separated and the orbital frequency is $\approx$ 500 cycles/sec (i.e. the gravitational wave frequency is approximately 1000 Hz). The orbital frequency at which the dynamical instability occurs (i.e. the orbital frequency at the innermost stable circular orbit) shows modest sensitivity to the neutron-star equation of state (particularly the mass-radius ratio, $M/R_o$, of the stars). This suggests that information about the equation of state of nuclear matter is encoded in the gravitational waves emitted just prior to the merger.

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References

Forward citations

Cited by 5 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Measuring gravitational waves from binary black hole coalescences: I. Signal to noise for inspiral, merger, and ringdown
gr-qc 1997-01 accept novelty 7.0 of 10

Binary black hole coalescences should be visible to initial LIGO out to roughly 200 to 250 Mpc and to LISA out to cosmological distances, with the optimal search phase shifting from inspiral to merger or ringdown as t...
Non-parametric inference of the neutron star equation of state from gravitational wave observations
gr-qc 2018-11 conditional novelty 6.0 of 10

A Gaussian-process prior over neutron-star equations of state, reweighted by GW170817, yields equation-of-state constraints whose spread is dominated by the choice of prior.
Tidal deformability of neutron stars with realistic equations of state and their gravitational wave signatures in binary inspiral
astro-ph.HE 2009-11 accept novelty 6.0 of 10

Tidal deformability of neutron stars spans an order of magnitude across realistic equations of state, but Advanced LIGO at 100 Mpc can only constrain unusually stiff ones; the Einstein Telescope could measure it cleanly.
Measuring the neutron star equation of state with gravitational wave observations
gr-qc 2009-01 conditional novelty 6.0 of 10

Five numerical binary neutron-star inspirals with different equations of state produce waveform differences from point-particle inspiral large enough to measure at 100 Mpc, implying neutron-star radius could be pinned...
Measuring gravitational waves from binary black hole coalescences: II. the waves' information and its extraction, with and without templates
gr-qc 1997-10 conditional novelty 6.0 of 10

Merger-phase gravitational waves carry roughly 10 to 60 bits of source information for LIGO/VIRGO and up to 200 for LISA, and templates must meet a stated accuracy criterion to preserve it.

How the literature uses it

8 arXiv papers cite this in 9 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 method or tool 1 paper

The dynamical equations for such a system can be expressed as follows [ref] : [equation] In the above, $M_t=M+M'$ is the total mass, $A_1, A_2$ and $A_3$ are dimensionless functions of $a_1,a_2,a_3$ as defined in Section 17 of Ref. [ref] .

Evolution of inspiralling neutron star binaries: effects of tidal interactions and orbital eccentricities · Dynamical equations of inspiraling NS binary · 0.88

Cites it as background 2 papers

Tidal effects on the gravitational waveform in circular neutron star (NS) binary inspirals have been studied extensively [ref] , including quasi-equilibrium tides [ref] and resonant tides [ref] .

Evolution of inspiralling neutron star binaries: effects of tidal interactions and orbital eccentricities · Introduction · 0.96
Furthermore, it is utilized in various contexts, such as dynamical instability of neutron-star binaries [ref] , gravitational instabilities in hydrodynamic fluid [ref] , post-Newtonian effects in magnetohydrodynamics [ref] and its role in the gravitational radiation by magnetic field of magnetars [ref] .

Accretion flows around spinning compact objects in the post-Newtonian regime · Introduction · 0.87

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