Coupling of Radial and Axial non-Radial Oscillations of Compact Stars: Gravitational Waves from first-order Differential Rotation

A. Nagar; A. Passamonti; C. F. Sopuerta; L. Gualtieri; M. Bruni

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Coupling of Radial and Axial non-Radial Oscillations of Compact Stars: Gravitational Waves from first-order Differential Rotation

A. Passamonti, M. Bruni, L. Gualtieri, A. Nagar, C. F. Sopuerta

General Relativity and Quantum Cosmology · Submitted 31 Dec 2005

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

The authors' main claim Of particular interest is the occurrence of signal amplifications in the form of resonance phenomena when a frequency associated with the radial pulsations is close to a frequency associated with one of the axial w-modes of the star.

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arXiv IDgr-qc/0601001 (version 1)

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CitationA. Nagar, A. Passamonti, C. F. Sopuerta, L. Gualtieri, M. Bruni. "Coupling of Radial and Axial non-Radial Oscillations of Compact Stars: Gravitational Waves from first-order Differential Rotation." arXiv:gr-qc/0601001 (2005). https://pith.science/paper/R6EZBWXO

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What the abstract itself states, as probabilities: claims first 0.07 · states limitation 0.62 · human participants 0.01 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.05 · compares with prior results 0.06 · mentions code or data availability 0.02.

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We investigate the non-linear coupling between radial and non-radial oscillations of static spherically symmetric neutron stars as a possible mechanism for the generation of gravitational waves that may lead to observable signatures. In this paper we concentrate on the axial sector of the non-radial perturbations. By using a multi-parameter perturbative framework we introduce a complete description of the non-linear coupling between radial and axial non-radial oscillations; we study the gauge invariant character of the associated perturbative variables and develop a computational scheme to evolve the non-linear coupling perturbations in the time domain. We present results of simulations corresponding to different physical situations and discuss the dynamical behaviour of this non-linear coupling. Of particular interest is the occurrence of signal amplifications in the form of resonance phenomena when a frequency associated with the radial pulsations is close to a frequency associated with one of the axial w-modes of the star. Finally, we mention possible extensions of this work and improvements towards more astrophysically motivated scenarios.

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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 investigate the non-linear coupling between radial and non-radial oscillations of static spherically symmetric neutron stars as a possible mechanism for the generation of gravitational waves that may lead to observable signatures.	contribution 0.90	0.83	0.13	hedged possibility 0.99
s1	In this paper we concentrate on the axial sector of the non-radial perturbations.	contribution 0.51	0.67	0.03	asserted 0.86
s2	By using a multi-parameter perturbative framework we introduce a complete description of the non-linear coupling between radial and axial non-radial oscillations; we study the gauge invariant character of the associated perturbative variables and develop a computational scheme to evolve the non-linear coupling perturbations in the time domain.	method 0.71	0.96	0.07	asserted 1.00
s3	We present results of simulations corresponding to different physical situations and discuss the dynamical behaviour of this non-linear coupling.	contribution 0.76	0.94	0.05	asserted 0.86
s4	Of particular interest is the occurrence of signal amplifications in the form of resonance phenomena when a frequency associated with the radial pulsations is close to a frequency associated with one of the axial w-modes of the star.	result 0.97	0.84	0.51	asserted 0.93
s5	Finally, we mention possible extensions of this work and improvements towards more astrophysically motivated scenarios.	future work 1.00	0.28	0.03	hedged possibility 0.56

What kind of paper the classifier reports this is: simulation study 0.60 · evidence from simulation or computation 1.00.

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Original abstract

We investigate the non-linear coupling between radial and non-radial oscillations of static spherically symmetric neutron stars as a possible mechanism for the generation of gravitational waves that may lead to observable signatures. In this paper we concentrate on the axial sector of the non-radial perturbations. By using a multi-parameter perturbative framework we introduce a complete description of the non-linear coupling between radial and axial non-radial oscillations; we study the gauge invariant character of the associated perturbative variables and develop a computational scheme to evolve the non-linear coupling perturbations in the time domain. We present results of simulations corresponding to different physical situations and discuss the dynamical behaviour of this non-linear coupling. Of particular interest is the occurrence of signal amplifications in the form of resonance phenomena when a frequency associated with the radial pulsations is close to a frequency associated with one of the axial w-modes of the star. Finally, we mention possible extensions of this work and improvements towards more astrophysically motivated scenarios.

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9 arXiv papers cite this in 9 sentences

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In this way, the oscillation frequencies of such stars, namely, $f$- and $p$-modes [ref] , would give us information about the composition and internal structure of such spherical objects (check, e.g., [ref] and their references).

Fluid pulsation modes and tidal deformability of anisotropic strange stars in light of the GW$170817$ event · Introduction · 0.84
As is well know, in GR radial oscillations of relativistic stars do not source gravitational wave (GW) emissions (although in principle they can couple to non-radial modes [ref] and potentially be observable during the post-merger phase [ref] ).

Dynamical Chameleon Neutron Stars: stability, radial oscillations and scalar radiation in spherical symmetry · Introduction · 0.89

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