A generalization of the Zerilli master variable for a dynamical spherical spacetime

David Brizuela

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A generalization of the Zerilli master variable for a dynamical spherical spacetime

David Brizuela

General Relativity and Quantum Cosmology · Submitted 20 May 2015

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

The authors' main claim In particular, two master variables are obtained: one corresponding to the polar mode of the gravitational wave, whereas the other encodes the complete physical information about the perturbative matter degree of freedom.

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What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.20 · human participants 0.01 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.04 · compares with prior results 0.24 · mentions code or data availability 0.01.

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

The evolution of polar perturbations on a spherical background spacetime is analyzed. The matter content is assumed to be a massless scalar field.This provides a nontrivial dynamics to the background and the linearized equations of motion become much more involved than in the vacuum case. The analysis is performed in a Hamiltonian framework, which makes explicit the dynamical role of each of the variables. After performing a number of canonical transformations, it is possible to completely decouple the different perturbative degrees of freedom into constrained, pure-gauge and gauge-invariant variables. In particular, two master variables are obtained: one corresponding to the polar mode of the gravitational wave, whereas the other encodes the complete physical information about the perturbative matter degree of freedom. The evolution equations for these master variables are obtained and simplified.

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#	sentence	role	the authors' own work	states the main conclusion	strength
s0	The evolution of polar perturbations on a spherical background spacetime is analyzed.	contribution 0.58	0.83	0.04	asserted 0.95
s1	The matter content is assumed to be a massless scalar field.This provides a nontrivial dynamics to the background and the linearized equations of motion become much more involved than in the vacuum case.	method 0.47	0.43	0.04	asserted 1.00
s2	The analysis is performed in a Hamiltonian framework, which makes explicit the dynamical role of each of the variables.	method 0.99	0.86	0.03	asserted 1.00
s3	After performing a number of canonical transformations, it is possible to completely decouple the different perturbative degrees of freedom into constrained, pure-gauge and gauge-invariant variables.	method 0.61	0.92	0.20	hedged possibility 0.54
s4	In particular, two master variables are obtained: one corresponding to the polar mode of the gravitational wave, whereas the other encodes the complete physical information about the perturbative matter degree of freedom.	result 0.91	0.92	0.62	asserted 1.00
s5	The evolution equations for these master variables are obtained and simplified.	result 0.63	0.94	0.19	asserted 1.00

What kind of paper the classifier reports this is: theoretical result 0.99 · evidence from proof or derivation 1.00.

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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

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Original abstract

The evolution of polar perturbations on a spherical background spacetime is analyzed. The matter content is assumed to be a massless scalar field.This provides a nontrivial dynamics to the background and the linearized equations of motion become much more involved than in the vacuum case. The analysis is performed in a Hamiltonian framework, which makes explicit the dynamical role of each of the variables. After performing a number of canonical transformations, it is possible to completely decouple the different perturbative degrees of freedom into constrained, pure-gauge and gauge-invariant variables. In particular, two master variables are obtained: one corresponding to the polar mode of the gravitational wave, whereas the other encodes the complete physical information about the perturbative matter degree of freedom. The evolution equations for these master variables are obtained and simplified.

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3 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 · 4 sentences without a confident label

Builds on it 2 papers

Our result generalizes previous works in the Hamiltonian formalism by Moncrief [ref] to arbitrary spherically symmetric backgrounds and arrives at a much simplified version of the physical Hamiltonian found in [ref] upon performing suitable canonical transformations.

Quantum Field Theory of Black Hole Perturbations with Backreaction II. Spherically symmetric 2nd order Einstein sector · Conclusion · 0.95
With the help of additional canonical transformations we simplify the reduced Hamiltonian as compared to [ref] .

Quantum Field Theory of Black Hole Perturbations with Backreaction IV. Spherically symmetric 2nd order Einstein-Maxwell sector in generalised gauges · Introduction · 0.84

Compares with it 1 paper

In another paper of this series [ref] we also consider purely geometrical perturbations in generalised gauges in order to compare our formalism with the general gauge formulations of [ref] .

Quantum Field Theory of Black Hole Perturbations with Backreaction II. Spherically symmetric 2nd order Einstein sector · Introduction · 0.87

Cites it as background 1 paper

Similar works have been done before in [ref] .

Quantum Field Theory of Black Hole Perturbations with Backreaction II. Spherically symmetric 2nd order Einstein sector · Perturbative expansion of the constraints · 0.88

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