Dynamical Tidal response of compact stars -- An EFT approach

Gregory Jarequi; Soumodeep Mitra; Varun Vaidya

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Dynamical Tidal response of compact stars -- An EFT approach

Gregory Jarequi, Soumodeep Mitra, Varun Vaidya

General Relativity and Quantum Cosmology · Submitted 12 Mar 2026

abstract compiled · 2026-09-24 · no language-model review

The authors' main claim This sets up a systematic framework for extracting the static and dynamical tidal love numbers(TLNs) to any order in the multipole expansion.

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We apply the point particle EFT approach to a compact star to systematically compute dynamical tidal love numbers for various non-rotating compact objects, extending the treatment of {arXiv:2307.10391[hep-th], arXiv:2407.08327 [gr-qc]}. We calculate the scattering amplitude in Black Hole Perturbation Theory(BPHT) for \textit{arbitrary} non-rotating compact stars using the Mano-Suzuki-Takasugi(MST) method with non zero surface reflectivity and match it with that obtained from point particle EFT order by order in the low frequency expansion. This sets up a systematic framework for extracting the static and dynamical tidal love numbers(TLNs) to any order in the multipole expansion. In this paper, we employ the technique to compute the Next-to-Next-to Leading Order TLN upto a universal constant and its Renormalization Group equation for non-viscous Neutron stars and Neutron stars admixed with Bosonic or Fermionic dark matter.

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#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We apply the point particle EFT approach to a compact star to systematically compute dynamical tidal love numbers for various non-rotating compact objects, extending the treatment of {arXiv:2307.10391[hep-th], arXiv:2407.08327 [gr-qc]}.	contribution 0.96	0.92	0.10	asserted 1.00
s1	We calculate the scattering amplitude in Black Hole Perturbation Theory(BPHT) for \textit{arbitrary} non-rotating compact stars using the Mano-Suzuki-Takasugi(MST) method with non zero surface reflectivity and match it with that obtained from point particle EFT order by order in the low frequency expansion.	method 0.93	0.93	0.13	asserted 1.00
s2	This sets up a systematic framework for extracting the static and dynamical tidal love numbers(TLNs) to any order in the multipole expansion.	contribution 0.46	0.66	0.21	asserted 1.00
s3	In this paper, we employ the technique to compute the Next-to-Next-to Leading Order TLN upto a universal constant and its Renormalization Group equation for non-viscous Neutron stars and Neutron stars admixed with Bosonic or Fermionic dark matter.	contribution 0.72	0.94	0.39	asserted 1.00

What kind of paper the classifier reports this is: theoretical result 0.71 · evidence from proof or derivation 0.89.

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Original abstract

We apply the point particle EFT approach to a compact star to systematically compute dynamical tidal love numbers for various non-rotating compact objects, extending the treatment of {arXiv:2307.10391[hep-th], arXiv:2407.08327 [gr-qc]}. We calculate the scattering amplitude in Black Hole Perturbation Theory(BPHT) for \textit{arbitrary} non-rotating compact stars using the Mano-Suzuki-Takasugi(MST) method with non zero surface reflectivity and match it with that obtained from point particle EFT order by order in the low frequency expansion. This sets up a systematic framework for extracting the static and dynamical tidal love numbers(TLNs) to any order in the multipole expansion. In this paper, we employ the technique to compute the Next-to-Next-to Leading Order TLN upto a universal constant and its Renormalization Group equation for non-viscous Neutron stars and Neutron stars admixed with Bosonic or Fermionic dark matter.

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References

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Renormalized dynamical tidal response of neutron stars in binary dynamics
gr-qc 2026-11 conditional novelty 6.0 of 10

A 4PM tidal response function for BSk22 neutron stars is extracted from scattering phases, matched to a harmonic oscillator model, and inserted into 3PN binary dynamics where it yields large post-Newtonian corrections...
Variational Approach to the Mathisson-Papapetrou-Dixon Equations of Motion for Extended Objects in General Relativity
gr-qc 2026-11 accept novelty 5.0 of 10

A variational approach to the MPD equations yields a simplified formula for the energy-momentum tensor and identifies the natural basis of curvature tensors conjugate to multipole moments.

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2 arXiv papers cite this in 3 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 · 2 sentences without a confident label

Cites it as background 1 paper

Dynamical tidal effects in compact binaries have been investigated in EFT approaches in Refs. [ref] .

Dynamical tidal response of neutron stars: From effective field theory to gravitational waveforms · Introduction · 0.98

What it cites · 87 sentences without a confident label

Contests 1 paper

In the near-zone, we make a change of variable to $x = r_H - r/r_H$, with the general solution of RW equation in this region can be written in terms of hypergeometric functions as, [equation] where, we have defined, [equation] where,$ϵ= 2 GM ω$, $_2F_1$ is the hypergeometric function and the arguments are given by, $a = -n-ν+s- i ϵ, b= n + ν+s+1 -iϵ, c = 1- 2 i ϵ$.[In the expression [ref], we have corrected a mistype in eqn. 3.23 of [ref] .] Further, $N = Γ(1 - s- 2 i ϵ)/Γ(-ν- i ϵ) Γ(1+ ν- i ϵ)$ is a normalization constant.

High-order Tail in Schwarzschild Space-time · MST method for scattering amplitude · contest 0.82

Builds on 1 paper

We first improve the result in [ref] to NNLO, computing the static and lowest dynamical TLN for a NS with no viscosity (hence zero dissipation).

Investigating tidal heating in neutron stars via gravitational Raman scattering · Introduction · 0.85

Uses the method or tool of 12 papers

These problems can be solved by using a worldline effective field theory (wEFT) or point particle EFT approach [ref] (see [ref] for review), as has been recently shown by [ref] in the case of rotating BH and non-rotating NS.

Towers of Gravitational Theories · Introduction · 0.81
These problems can be solved by using a worldline effective field theory (wEFT) or point particle EFT approach [ref] (see [ref] for review), as has been recently shown by [ref] in the case of rotating BH and non-rotating NS.

The Effective Field Theorist's Approach to Gravitational Dynamics · Introduction · 0.81
These problems can be solved by using a worldline effective field theory (wEFT) or point particle EFT approach [ref] (see [ref] for review), as has been recently shown by [ref] in the case of rotating BH and non-rotating NS.

Revisiting the matching of black hole tidal responses: a systematic study of relativistic and logarithmic corrections · Introduction · 0.81

Uses data or values from 1 paper

The renormalised angular momentum $ν$ and the coefficients $a^ν_n$ up to this order is given in [ref] , and we have taken the same for our calculation in this paper.

High-order Tail in Schwarzschild Space-time · MST method for scattering amplitude · 0.96

Compares with 2 papers

[equation] These equations match with [ref] up to some differences in convention.

Tidal Love numbers of neutron stars · Solution at $O(ω^0)$ · 1.00
However, in the following we will keep viscosity related terms in the calculation up until $ω^6$ order(NLO), to match our results with previous tidal dissipation number calculated in [ref] .

Investigating tidal heating in neutron stars via gravitational Raman scattering · Solving stellar interior · 0.94

Cites as support 2 papers

Further, [ref] has shown that neglecting dynamical tides results in large biases in estimation of nuclear properties of NS.

Impact of Dynamical Tides on the Reconstruction of the Neutron Star Equation of State · Introduction · 1.00
GW observations effectively rule out such halos created by even small percentages of fermionic dark matter [ref] .

Comprehensive study of compact stars with dark matter · Neutron stars admixed with fermionic dark matter · 0.98

Cites as background 16 papers

We start with a brief review of the point particle EFT formalism for compact objects [ref] .

An Effective Field Theory of Gravity for Extended Objects · The EFT action · 0.84
We start with a brief review of the point particle EFT formalism for compact objects [ref] .

Towers of Gravitational Theories · The EFT action · 0.84
Although most studies on TLN, especially for NS and DM admixed NS systems (see [ref] for some treatment of beyond static TLNs in NS) focus on the static regime, in recent years interest in higher order tidal responses has been growing steadily.

New perspectives on neutron star and black hole spectroscopy and dynamic tides · Introduction · 0.85

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