A Strong Cosmologically Coupled Mass Growth Solution in Linearized General Relativity

@misc{croker2026strong,
  title = {{A Strong Cosmologically Coupled Mass Growth Solution in Linearized General Relativity}},
  author = {Kevin S. Croker and Joshua Cohon and Viktor T. Toth and Massimiliano Rinaldi and Nicolas Fernandez and Joel L. Weiner and Duncan Farrah and Gregory Tarlé and Gustavo Niz and Christopher Cain and James W. Rohlf and Alejandro Aviles and Jake Summers and Leander Thiele and Rogier A. Windhorst and Joshua Grumski-Flores},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.38303},
  eprint = {2609.38303},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.38303},
}

TY  - UNPB
TI  - A Strong Cosmologically Coupled Mass Growth Solution in Linearized General Relativity
AU  - Kevin S. Croker
AU  - Joshua Cohon
AU  - Viktor T. Toth
AU  - Massimiliano Rinaldi
AU  - Nicolas Fernandez
AU  - Joel L. Weiner
AU  - Duncan Farrah
AU  - Gregory Tarlé
AU  - Gustavo Niz
AU  - Christopher Cain
AU  - James W. Rohlf
AU  - Alejandro Aviles
AU  - Jake Summers
AU  - Leander Thiele
AU  - Rogier A. Windhorst
AU  - Joshua Grumski-Flores
PY  - 2026
DA  - 2026/09/29
PB  - arXiv
DO  - 10.48550/arxiv.2609.38303
UR  - https://arxiv.org/abs/2609.38303
AB  - DESI Data Release 2 has heightened interest in cosmologically coupled black holes (CCBHs) as an explanation for accelerating late-time expansion, but known models for CCBHs grow too slowly to drive it. We construct at linear order a solution to General Relativity whose Hernandez-Misner-Sharp mass passively grows ∝ a^κ as the universe expands. The constant κ enters all eigenvalues of the Weyl and stress-tensor operators, so growth is unambiguously physical in both free-field and material sectors. The solution is causal over spacetime relevant for stellar collapse compact objects. A cloud of energized vacuum emerges at κ= 3, complementing the a^3 scaling predicted elsewhere for the masses of energized vacuum black holes. This first step toward κ∼ 3 CCBH exact solutions enables observational tests with pulsar binaries.
ER  -