What question did this study set out to answer?

The aim is to correct the compactness of CCEGA black stars and confirm their rotational stability with new parameters.

May 25, 2026Open Access

P51 v2.0: Rotational Stability of CCEGA Black Stars — Corrected Compactness C = 0.63, Ergoregion Outside Object

Key Points

The aim is to correct the compactness of CCEGA black stars and confirm their rotational stability with new parameters.
Analytical verification of compactness values using corrected density ratios
Assessment of ergoregion and rotational dynamics in black stars of 4.56-12.0 M☉
Evaluation of rotational frequencies and light ring positions
Corrected compactness value ranges from 0.63 to 1.27 based on density ρ_c = 7.4 ρ_nuc
Confirmed light ring position at r = 3GM/c² and stable ergosphere structure across masses
Maximum rotation measured between 0.76 and 2.0 kHz with no ergoregion instability

Abstract

Correction to v1. 0. C = 0. 44 was incorrect (used ρc ≈ 2. 6 ρₙuc implicitly). Correct value with ρc = 7. 4 ρₙuc gives C ≈ 0. 63–1. 27. Ergoregion is exterior to the object for all masses. Ergoregion instability claim retracted. Rotational stability recovered via P60 (geometric suppression mechanism). Analytical verification that CCEGA black stars (4. 56–12. 0 M☉, C ≈ 0. 44) are rotationally stable. Light ring confirmed at r = 3GM/c². Ergosphere buried inside stellar surface for all masses at maximum spin. No Friedman (1978) ergoregion instability. Maximum rotation 0. 76–2. 0 kHz. Stability is structural consequence of ρc = 7. 4 ρₙuc. Keywords: CCEGA, black stars, ergoregion instability, light ring, rotation, compact objects, angular momentum

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