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General-relativistic electromagnetic fields around a slowly rotating neutron star: time-dependent pseudo-spectral simulations

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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J. Pétri

High Energy Astrophysical Phenomena · Submitted 7 Jan 2014

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

The authors' main claim Stationary solutions are readily obtained and compared to semi-analytical calculations.

how it is stated · asserted 0.95 read the record →

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arXiv ID1401.1367 (version 1)
Pith ID7XPRB72W, Pith's permanent record of this paper and its review
CitationJ. P\'etri. "General-relativistic electromagnetic fields around a slowly rotating neutron star: time-dependent pseudo-spectral simulations." arXiv:1401.1367 (2014). https://pith.science/paper/7XPRB72W
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The compiled record

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, 7,346 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.28 · states limitation 0.34 · human participants 0.01 · controlled comparison 0.16 · randomized assignment 0.01 · states quantitative result 0.05 · compares with prior results 0.90 · mentions code or data availability 0.03.

The abstract, sentence by sentence

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

Pulsars are believed to loose their rotational kinetic energy primarily by a large amplitude low frequency electromagnetic wave which is eventually converted into particle creation, acceleration and followed by a broad band radiation spectrum. To date, there exist no detailed calculation of the exact spin-down luminosity with respect to the neutron star magnetic moment and spin frequency, including general-relativistic effects. Estimates are usually given according to the flat spacetime magnetodipole formula. The present paper pursue our effort to look for accurate solutions of the general-relativistic electromagnetic field around a slowly rotating magnetized neutron star. In a previous work, we already found approximate stationary solutions to this problem. Here we address again this problem but using a more general approach. We indeed solve the full set of time-dependent Maxwell equations in a curved vacuum space-time following the 3+1 formalism. The numerical code is based on our pseudo-spectral method exposed in a previous paper for flat space-time. We adapted it to an arbitrary fixed background metric. Stationary solutions are readily obtained and compared to semi-analytical calculations.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Pulsars are believed to loose their rotational kinetic energy primarily by a large amplitude low frequency electromagnetic wave which is eventually converted into particle creation, acceleration and followed by a broad band radiation spectrum. background 1.00 0.04 0.04 hedged possibility 0.87
s1 To date, there exist no detailed calculation of the exact spin-down luminosity with respect to the neutron star magnetic moment and spin frequency, including general-relativistic effects. gap 1.00 0.06 0.04 asserted 1.00
s2 Estimates are usually given according to the flat spacetime magnetodipole formula. background 0.95 0.04 0.02 asserted 0.99
s3 The present paper pursue our effort to look for accurate solutions of the general-relativistic electromagnetic field around a slowly rotating magnetized neutron star. contribution 0.98 0.58 0.05 asserted 0.87
s4 In a previous work, we already found approximate stationary solutions to this problem. background 0.88 0.88 0.02 asserted 1.00
s5 Here we address again this problem but using a more general approach. contribution 0.79 0.55 0.03 asserted 0.95
s6 We indeed solve the full set of time-dependent Maxwell equations in a curved vacuum space-time following the 3+1 formalism. method 0.82 0.94 0.09 asserted 1.00
s7 The numerical code is based on our pseudo-spectral method exposed in a previous paper for flat space-time. method 1.00 0.67 0.02 asserted 1.00
s8 We adapted it to an arbitrary fixed background metric. method 0.96 0.90 0.03 asserted 1.00
s9 Stationary solutions are readily obtained and compared to semi-analytical calculations. result 0.50 0.85 0.11 asserted 0.95

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

What was examined, and what was not

sources read
  • arXiv listing abstract v1
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

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

Pulsars are believed to loose their rotational kinetic energy primarily by a large amplitude low frequency electromagnetic wave which is eventually converted into particle creation, acceleration and followed by a broad band radiation spectrum. To date, there exist no detailed calculation of the exact spin-down luminosity with respect to the neutron star magnetic moment and spin frequency, including general-relativistic effects. Estimates are usually given according to the flat spacetime magnetodipole formula. The present paper pursue our effort to look for accurate solutions of the general-relativistic electromagnetic field around a slowly rotating magnetized neutron star. In a previous work, we already found approximate stationary solutions to this problem. Here we address again this problem but using a more general approach. We indeed solve the full set of time-dependent Maxwell equations in a curved vacuum space-time following the 3+1 formalism. The numerical code is based on our pseudo-spectral method exposed in a previous paper for flat space-time. We adapted it to an arbitrary fixed background metric. Stationary solutions are readily obtained and compared to semi-analytical calculations.

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References
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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

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