Probing Quantum Gravity effects with Extreme Mass Ratio Inspirals around Rotating Hayward Black Holes

Abstract: We investigate extreme mass-ratio inspirals (EMRIs) around a rotating Hayward black hole to assess the detectability of signatures arising from quantum gravity.The quantum parameter $α_0$, which encodes deviations from general relativity (GR), introduces extra correction terms in both the orbital frequency and the fluxes. Our results show that after one year of accumulated observation, these corrections induce a detectable dephasing in the EMRI waveform. Using the modified orbital evolution driven by $α_0$, we generate waveforms via the augmented analytic kludge (AAK) model implemented in the \texttt{FastEMRIWaveforms} package. Furthermore, we utilize the time-delay interferometry (TDI) to suppress the laser noise and phase fluctuations induced by spacecraft motion, and then employ the Fisher information matrix (FIM) to test the sensitivity of LISA in detecting deviations from GR. Our results demonstrate the potential of LISA to probe quantum-gravity effects through high-precision observations of EMRIs.

• The paper develops a pipeline combining rotating Hayward geodesics, quantum-corrected fluxes, AAK waveforms, LISA TDI channels, and Fisher analysis to test deviations from Kerr.
• The analysis finds that quantum corrections accumulate into measurable one-year EMRI dephasing, with spin amplifying the effect through the coupling between rotation and the Hayward parameter α₀.
• For a 10⁶-solar-mass primary, 10-solar-mass secondary, and SNR 150, the forecast uncertainty is σ(α₀)=3.07×10⁻⁴, although weak-field fluxes and leading-order adiabatic modeling limit robustness.

Overview

This paper assesses whether LISA observations of extreme mass-ratio inspirals (EMRIs) can detect quantum-gravity corrections encoded in a rotating Hayward regular black hole (HBH). The central object is characterized by the regularization parameter $\alpha_0$, which replaces the central singularity with a Planck-scale de Sitter core and vanishes in the Schwarzschild/Kerr limit. The authors derive quantum-corrected orbital frequencies and radiation fluxes for eccentric equatorial orbits, propagate the orbital evolution adiabatically, generate augmented analytic kludge (AAK) waveforms via the FastEMRIWaveforms (FEW) package, and quantify parameter-estimation sensitivity using time-delay interferometry (TDI) observables combined with a Fisher information matrix (FIM) analysis. The headline result is that one year of observation yields measurable waveform dephasing, and that LISA can constrain $\alpha_0$ to $\Delta\alpha_0 = 3.07\times10^{-4}$ at SNR $= 150$.

Rotating Hayward spacetime and its phase structure

The static Hayward metric uses the mass function $m(r) = Mr^3/(r^3 + \alpha_0 M)$, reducing to Schwarzschild as $\alpha_0 \to 0$. The rotating generalization follows Bambi–Modesto via the Newman–Janis algorithm. A key structural feature emphasized by the authors is that rotation introduces a non-trivial coupling between $\alpha_0$ and the spin $a$: the existence condition for horizons ($\Delta = r^2 - 2m(r)r + a^2 > 0$) restricts the allowed $(a/M,\,\alpha_0/M^2)$ region, with the maximum admissible $\alpha_0$0 decreasing monotonically with spin and recovering the static bound $\alpha_0$1 at $\alpha_0$2. This coupling is absent in the static model and, as shown below, amplifies the observable impact of quantum corrections.

Quantum-corrected geodesics and fluxes

For equatorial motion ($\alpha_0$3), bound orbits are parametrized by semi-latus rectum $\alpha_0$4 and eccentricity $\alpha_0$5, with conserved $\alpha_0$6 and $\alpha_0$7 obtained analytically; setting $\alpha_0$8 recovers Kerr. Both fundamental frequencies admit expansions of the form $\alpha_0$9, where the GR pieces are computed with the KerrGeodesics package and the correction terms are given in closed form, scaling as $\Delta\alpha_0 = 3.07\times10^{-4}$0 and $\Delta\alpha_0 = 3.07\times10^{-4}$1 with explicit spin-dependent contributions.

The energy and angular momentum fluxes are similarly decomposed as GR plus $\Delta\alpha_0 = 3.07\times10^{-4}$2 terms. The GR fluxes use higher-order post-Newtonian expressions with Teukolsky-based phenomenological fits, while the quantum-corrected fluxes are computed with the quadrupole-octupole formula in the weak-field approximation, yielding polynomial-in-$\Delta\alpha_0 = 3.07\times10^{-4}$3 series in $\Delta\alpha_0 = 3.07\times10^{-4}$4 and $\Delta\alpha_0 = 3.07\times10^{-4}$5 (with spin-dependent pieces at $\Delta\alpha_0 = 3.07\times10^{-4}$6 and $\Delta\alpha_0 = 3.07\times10^{-4}$7). Because these corrections enter only at high post-Newtonian order, their per-cycle effect is small; detectability therefore rests entirely on cumulative accumulation over the long EMRI inspiral.

Orbital evolution, dephasing, and waveforms

Within the adiabatic approximation, flux balance determines $\Delta\alpha_0 = 3.07\times10^{-4}$8 and $\Delta\alpha_0 = 3.07\times10^{-4}$9 through the standard Jacobian inversion of the $= 150$0 relations. The authors compute the quadrupolar dephasing $= 150$1 and find that the azimuthal contribution dominates, so $= 150$2. Adopting $= 150$3 rad as the detection threshold for SNR $= 150$4, they show that dephasing grows with both $= 150$5 and, for fixed $= 150$6, with spin $= 150$7 — the rotational amplification anticipated from the $= 150$8–$= 150$9 coupling in the metric. After one year of accumulated observation, AAK waveforms generated with FEW for the fiducial system $m(r) = Mr^3/(r^3 + \alpha_0 M)$0 show visible deviations from the GR baseline for non-zero $m(r) = Mr^3/(r^3 + \alpha_0 M)$1.

TDI response and Fisher forecast

The data-analysis pipeline projects the strain onto all six LISA links using antenna pattern functions and first-order light-propagation approximations, constructs the first-generation Michelson combinations $m(r) = Mr^3/(r^3 + \alpha_0 M)$2 via delay operators, and forms the quasi-uncorrelated $m(r) = Mr^3/(r^3 + \alpha_0 M)$3 channels with the standard Marsat–Baker noise PSDs built from the oms and acc noise components. Since the $m(r) = Mr^3/(r^3 + \alpha_0 M)$4 channel responds weakly to the signal, the analysis retains only $m(r) = Mr^3/(r^3 + \alpha_0 M)$5 and $m(r) = Mr^3/(r^3 + \alpha_0 M)$6.

The FIM spans an eleven-parameter space $m(r) = Mr^3/(r^3 + \alpha_0 M)$7. For the fiducial configuration — $m(r) = Mr^3/(r^3 + \alpha_0 M)$8, $m(r) = Mr^3/(r^3 + \alpha_0 M)$9, $\alpha_0 \to 0$0, $\alpha_0 \to 0$1, $\alpha_0 \to 0$2, $\alpha_0 \to 0$3, fixed sky and inclination angles, luminosity distance tuned to SNR $\alpha_0 \to 0$4, and $\alpha_0 \to 0$5 chosen to guarantee one year of adiabatic evolution before plunge — the marginalized $\alpha_0 \to 0$6 uncertainty on the quantum parameter is:

Quantity	Value
Fiducial $\alpha_0 \to 0$7	$\alpha_0 \to 0$8
Forecast $\alpha_0 \to 0$9	$\alpha_0$0
Total SNR	$\alpha_0$1
Observation time	$\alpha_0$2 yr

This sub-milliparameter precision implies that even if the true spacetime is exactly Kerr ($\alpha_0$3), LISA would bound deviations at the $\alpha_0$4 level for this source configuration, comparable in spirit to constraints obtainable on other modified-gravity parameters with EMRIs.

Limitations and open questions

The analysis operates at leading (adiabatic, 0PA) order and neglects self-force interactions between the secondary and its own perturbed field; the authors explicitly note, citing related work, that this omission can introduce systematic biases in parameter estimation, and defer higher-order (post-adiabatic) corrections to future work. Several further caveats bear directly on the quoted precision: the quantum-corrected fluxes are evaluated only in the weak-field quadrupole-octupole approximation rather than from Teukolsky-based computations on the HBH background; the FIM assumes Gaussian errors and a single source at fixed sky position and inclination; glitches, overlapping sources, and second-generation TDI effects are not modeled; and the constraint is reported for one fiducial system, so its dependence on mass ratio, spin, eccentricity, and SNR remains unquantified. Whether the $\alpha_0$5 measurement can be degenerate with environmental effects or with intrinsic-parameter shifts is not addressed.

Conclusion

The paper establishes a complete pipeline — from a rotating regular black hole metric through quantum-corrected orbital dynamics and kludge waveforms to TDI-based Fisher forecasts — demonstrating that Hayward-type quantum gravity corrections accumulate into detectable EMRI dephasing within a one-year LISA observation, with a projected sensitivity of $\alpha_0$6 at SNR 150. The result's robustness hinges on extending the flux calculation beyond the weak-field approximation and incorporating post-adiabatic self-force corrections, which remain open problems for quantitative forecasts of this kind.