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Superradiant and dynamical spin-down of neutron stars with gravitational wave implications

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Indra Kumar Banerjee, Sandeep Chatterjee, Biswarup Das, Ujjal Kumar Dey

High Energy Astrophysical Phenomena · Submitted 26 Dec 2025 · Published version

abstract compiled · 2026-09-25 · no language-model review

The authors' main claim We propose superradiant spin-down as a potential faster spin-down process.

how it is stated · hedged possibility 0.90 read the record →

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arXiv ID2512.21955 (version 2)
Pith IDKL2ROEWR, Pith's permanent record of this paper and its review
CitationBiswarup Das, Indra Kumar Banerjee, Sandeep Chatterjee, Ujjal Kumar Dey. "Superradiant and dynamical spin-down of neutron stars with gravitational wave implications." arXiv:2512.21955 (2025). https://pith.science/paper/KL2ROEWR
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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-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-25: 1 request, 4,235 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.12 · human participants 0.01 · controlled comparison 0.16 · randomized assignment 0.01 · states quantitative result 0.04 · compares with prior results 0.45 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

Neutron stars such as pulsars and magnetars lose angular momentum primarily through electromagnetic dipole radiation, gravitational waves, $r$-mode oscillation. However, spin variations, particularly enhanced spin-down rates, indicate additional spin-down mechanisms. We propose superradiant spin-down as a potential faster spin-down process. By modelling the interplay between conventional and superradiant spin-down channels, we evaluate their impact on neutron star rotational evolution. We also discuss gravitational-wave emission produced by quadrupole deformation, $r$-mode oscillations, and axion-induced bosonic clouds around an isolated neutron star, highlighting their potential as distinct multi-messenger probes in upcoming detectors.

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 Neutron stars such as pulsars and magnetars lose angular momentum primarily through electromagnetic dipole radiation, gravitational waves, $r$-mode oscillation. background 1.00 0.05 0.03 asserted 1.00
s1 However, spin variations, particularly enhanced spin-down rates, indicate additional spin-down mechanisms. background 0.51 0.09 0.05 hedged possibility 0.85
s2 We propose superradiant spin-down as a potential faster spin-down process. contribution 0.99 0.49 0.27 hedged possibility 0.90
s3 By modelling the interplay between conventional and superradiant spin-down channels, we evaluate their impact on neutron star rotational evolution. method 0.58 0.91 0.10 asserted 0.95
s4 We also discuss gravitational-wave emission produced by quadrupole deformation, $r$-mode oscillations, and axion-induced bosonic clouds around an isolated neutron star, highlighting their potential as distinct multi-messenger probes in upcoming detectors. contribution 0.80 0.45 0.13 hedged possibility 0.93

What kind of paper the classifier reports this is: theoretical result 0.85 · evidence from simulation or computation 0.61.

What was examined, and what was not

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  • references and citing sentences
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  • P abstract
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  • 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

Neutron stars such as pulsars and magnetars lose angular momentum primarily through electromagnetic dipole radiation, gravitational waves, $r$-mode oscillation. However, spin variations, particularly enhanced spin-down rates, indicate additional spin-down mechanisms. We propose superradiant spin-down as a potential faster spin-down process. By modelling the interplay between conventional and superradiant spin-down channels, we evaluate their impact on neutron star rotational evolution. We also discuss gravitational-wave emission produced by quadrupole deformation, $r$-mode oscillations, and axion-induced bosonic clouds around an isolated neutron star, highlighting their potential as distinct multi-messenger probes in upcoming detectors.

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What this paper does with the arXiv papers it cites

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

What it cites · 74 sentences without a confident label

Uses data or values from 4 papers
  • Fig. [ref] shows the spin frequency evolution with time, for different axion masses ($m_A$) and magnetic fields ($B$), where pulsar PSR J1748$–$2446ad is taken as reference ($f_0=716$ Hz) assuming $g_aγγ = 10^-12$ GeV$^-1$ with a conductivity for the magnetosphere $σ_MR$ = 0.1 [ref] .

    A Radio Pulsar Spinning at 716 Hz · Spin-down via superradiance · 0.99

  • Fig. [ref] shows the spin frequency evolution with time, for different axion masses ($m_A$) and magnetic fields ($B$), where pulsar PSR J1748$–$2446ad is taken as reference ($f_0=716$ Hz) assuming $g_aγγ = 10^-12$ GeV$^-1$ with a conductivity for the magnetosphere $σ_MR$ = 0.1 [ref] .

    Axion superradiance in rotating neutron stars · Spin-down via superradiance · 0.99

  • In Fig. [ref], $P$-$Ṗ$ distribution from ATNF pulsar catalogue [ref] is shown, with each data point representing a detected pulsar.

    The ATNF Pulsar Catalogue · Introduction · 1.00

Cites as support 2 papers
Cites as background 3 papers
  • Prior studies have considered axion production via non-stationary pair-plasma discharges near pulsar polar caps [ref] .

    Axion Clouds around Neutron Stars · GW signal due to superradiance · 0.82

  • Understanding how the spin evolves is key to interpreting existing observations and uncovering potential new astrophysical phenomena [ref] .

    Spin evolution of neutron stars · Introduction · 0.90

  • A key diagnostic of this evolution is the braking index $n$ which can be expressed as $n=ΩΩ̈/Ω̇^2$ [ref] , where \(Ω̇\) and \(Ω̈\) correspond to the first and second time derivatives of rotational spin angular frequency of the star, capturing the instantaneous spin-down rate.

    Pulsar Braking Indices Revisited · Introduction · 0.90

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