G(2) Glueball Boson Stars Reach C=0.3247 Compactness and Distinct Ringdown in Thomas-Fermi Limit
GC9 glueball stars achieve Kerr-like compactness and a distinct axial mode without horizons or light rings. The Thomas-Fermi EOS yields scale-independent observables fixed by Λ_T alone. The framework is falsifiable via gravitational-wave ringdown and compact-dark-matter searches.
The work solves the Tolman-Oppenheimer-Volkoff, Hinderer tidal, and Hartle-Thorne equations under a nonic-density closure that is bag-free and Q-ball stable. After Thomas-Fermi rescaling, macroscopic observables depend only on collective stiffness Λ_T, yielding maximum-mass values C=0.3247, Λ=4.37, and ĪC^{3/2}=0.947. The exterior Regge-Wheeler potential supports a genuine axial mode whose damping time is ~10% shorter and real frequency 24.1% higher than Schwarzschild, offering a potential discriminant for horizon-scale observations.
Moderate vector anisotropy alters static and first-order quantities by only a few percent, yet the full coupled spectrum remains unexplored. Cowling analysis isolates matter-supported quadrupolar modes, while the scalar-burst and seeded-collapse sections remain phenomenological. The multi-sector scenario requires distinct constant-Λ_T branches spanning keV supermassive to PeV asteroid-mass objects.
Existing boson-star literature (e.g., Liebling & Palenzuela 2017, arXiv:1202.5809) and recent LIGO-Virgo tidal constraints on exotic compact objects provide context; GC9 supplies a falsifiable, restricted Kerr-mimicry benchmark testable by future ringdown catalogs and microlensing surveys.
Next steps include full numerical-relativity evolutions of GC9 binaries and polarization-resolved waveforms to quantify deviations from Kerr at detector-relevant frequencies.
LIGO-Virgo-KAGRA O5: no GC9-like axial mode with |Im(ω)| 10% below Schwarzschild at SNR>20 by end of 2028
Sources (2)
- [1]Primary Source(https://arxiv.org/abs/2608.28688)
- [2]Supporting Source(https://arxiv.org/abs/1202.5809)