Black hole spin-mass correlation and vector resonant relaxation in gaseous star clusters: the origin of GW231123?

@misc{roupas2026black,
  title = {{Black hole spin-mass correlation and vector resonant relaxation in gaseous star clusters: the origin of GW231123?}},
  author = {Zacharias Roupas},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2607.17869},
  eprint = {2607.17869},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2607.17869},
}

TY  - UNPB
TI  - Black hole spin-mass correlation and vector resonant relaxation in gaseous star clusters: the origin of GW231123?
AU  - Zacharias Roupas
PY  - 2026
DA  - 2026/10/29
PB  - arXiv
DO  - 10.48550/arxiv.2607.17869
UR  - https://arxiv.org/abs/2607.17869
AB  - During the formation of a star cluster a spin-mass correlation of stellar black holes is generated as they grow via accretion of the residual gas. Moreover, the black hole spin tends to be anti-aligned with its orbital angular momentum in the cluster. We show that GW231123, reported by the LIGO-Virgo-KAGRA (LVK) collaboration, lies on our predicted high-mass, high-spin plateau of the spin-mass correlation with positive Bayesian evidence over the LVK prior. Furthermore, vector resonant relaxation (VRR) equilibrium is favored over the isotropic LVK prior in reproducing the distribution of the relative spin tilt. The joint Bayes factor suggests strong evidence for the favored cluster models. GW231123 is thus consistent with our proposed channel that generates correlated black hole masses and spins, and drives the spins' orientations.
ER  -