What question did this study set out to answer?

To compute and analyze the tidal deformability Λ of CCEGA black stars, contrasting it with general relativity black holes.

May 26, 2026Open Access

P65: Tidal Deformability of CCEGA Black Stars — Λ ≠ 0 as a Surface Signature

Key Points

To compute and analyze the tidal deformability Λ of CCEGA black stars, contrasting it with general relativity black holes.
Computed tidal deformability Λ_BS for CCEGA black stars across a range of masses (4.56–14.75 M☉).
Evaluated frequency independence of Λ_BS during inspiral phases, particularly under chirp conditions.
Findings indicate Λ_BS ≈ 0.005–0.66, which is nonzero unlike GR black holes where Λ_BH = 0.
For neutron stars, Λ predicts ≈ 377–538, consistent with LIGO observations from GW170817 (within 90% CI).
Stacking of ~100 mass-gap mergers may detect Λ̃ ~ 0.3 statistically.

Abstract

We compute the tidal deformability Λ of CCEGA black stars. Two results: (1) ΛBS is frequency-independent during inspiral — fISCO < fcut throughout the chirp. (2) ΛBS ≈ 0. 005–0. 66 for masses 4. 56–14. 75 M☉, nonzero in contrast to GR black holes (ΛBH = 0). For normal neutron stars, CCEGA predicts Λ ≈ 377–538 for M = 1. 4 M☉, consistent with GW170817 (within 90% CI). A mild tension exists at the upper end, constraining k₂CCEGA ≲ 0. 07. ET stacking of ~100 mass-gap mergers could detect Λ̃ ~ 0. 3 statistically.

P65: Tidal Deformability of CCEGA Black Stars — Λ ≠ 0 as a Surface Signature

Key Points

Abstract

Cite This Study