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Triaxial instabilities in rapidly rotating Neutron Stars
High Energy Astrophysical Phenomena · Submitted 5 Dec 2017
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These instabilities set a more rigorous limit to the rotation frequency of neutron star than the Kepler frequency/mass shedding limit.
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The abstract, sentence by sentence
Viscosity driven bar mode secular instabilities of rapidly rotating neutron stars are studied using LORENE/Nrotstar code. These instabilities set a more rigorous limit to the rotation frequency of neutron star than the Kepler frequency/mass shedding limit. The procedure employed in the code comprises of perturbing an axisymmetric and stationary configuration of a neutron star and studying its evolution by constructing a series of triaxial quasi-equilibrium configurations. Symmetry breaking point was found out for Polytropic as well as 10 realistic Equations of states (EOS) from the CompOSE database. The concept of piecewise polytropic EOSs has been used to comprehend the rotational instability of Realistic EOSs and validated with 19 different Realistic EOSs from CompOSE. The possibility of detecting quasi-periodic gravitational waves from viscosity driven instability with ground based LIGO/VIRGO interferometers is also discussed very briefly.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Viscosity driven bar mode secular instabilities of rapidly rotating neutron stars are studied using LORENE/Nrotstar code. | contribution 0.65 | 0.87 | 0.05 | asserted 0.98 |
| s1 | These instabilities set a more rigorous limit to the rotation frequency of neutron star than the Kepler frequency/mass shedding limit. | interpretation 0.57 | 0.37 | 0.63 | asserted 1.00 |
| s2 | The procedure employed in the code comprises of perturbing an axisymmetric and stationary configuration of a neutron star and studying its evolution by constructing a series of triaxial quasi-equilibrium configurations. | method 1.00 | 0.84 | 0.04 | asserted 0.98 |
| s3 | Symmetry breaking point was found out for Polytropic as well as 10 realistic Equations of states (EOS) from the CompOSE database. | result 0.81 | 0.92 | 0.07 | asserted 1.00 |
| s4 | The concept of piecewise polytropic EOSs has been used to comprehend the rotational instability of Realistic EOSs and validated with 19 different Realistic EOSs from CompOSE. | method 0.87 | 0.83 | 0.08 | asserted 1.00 |
| s5 | The possibility of detecting quasi-periodic gravitational waves from viscosity driven instability with ground based LIGO/VIRGO interferometers is also discussed very briefly. | interpretation 0.69 | 0.29 | 0.04 | hedged possibility 0.87 |
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The paper
Original abstract
Viscosity driven bar mode secular instabilities of rapidly rotating neutron stars are studied using LORENE/Nrotstar code. These instabilities set a more rigorous limit to the rotation frequency of neutron star than the Kepler frequency/mass shedding limit. The procedure employed in the code comprises of perturbing an axisymmetric and stationary configuration of a neutron star and studying its evolution by constructing a series of triaxial quasi-equilibrium configurations. Symmetry breaking point was found out for Polytropic as well as 10 realistic Equations of states (EOS) from the CompOSE database. The concept of piecewise polytropic EOSs has been used to comprehend the rotational instability of Realistic EOSs and validated with 19 different Realistic EOSs from CompOSE. The possibility of detecting quasi-periodic gravitational waves from viscosity driven instability with ground based LIGO/VIRGO interferometers is also discussed very briefly.
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What this paper does with the arXiv papers it cites
What it cites · 6 sentences without a confident label
Uses the method or tool of 2 papers
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The theoretical model used for the numerical code has been described at length in [ref] , [ref] , [ref] , [ref] , [ref] and [ref] .
An introduction to the theory of rotating relativistic stars · Theoretical Model · 1.00
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A detailed description of parameterization of realistic EOSs [ref] into piece-wise polytropic EOSs, the choice of parameters and fitting routines have been provided in [ref] .
Equations of state for supernovae and compact stars · Piecewise Polytropic EOSs · 0.86
Cites as background 1 paper
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This can be attributed to the fact that EOSs must be stiff enough for bifurcation to occur at an angular velocity lower than that of maximum angular velocity ($Ω_k$) [ref] for which a stationary solution exists [ref] . $Ω_k$ is reached when the centrifugal force is exactly equal in magnitude to the gravitational potential energy at the equator of the star. $Ω_k$ is also known as the Keplerian velocity (mass-shedding limit) [ref] .
The Physics of Neutron Stars · Introduction · 0.85
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