Parameter Space, Realistic Matter, and Universal Relations in Bose--Einstein Condensate Dark Stars
Abstract
We study slowly rotating Bose--Einstein condensate (BEC) dark stars by solving the Tolman--Oppenheimer--Volkoff, Hartle dipole, and Postnikov--Hinderer equations together for a polytropic equation of state with a Lee--Huang--Yang correction of strength ζ~\citep{Panotopoulos2026}. A continuous scan of ζ from 0 to 1.5 shows the mean-field-to-corrected transition is smooth, with no hidden structure at intermediate values. Scanning the underlying boson parameters (m,as) more broadly, we find that a 2 M⊙ maximum-mass bound and a GW170817-like tidal bound Λ1.4≲800 cannot be satisfied simultaneously anywhere in this equation-of-state class. The I-Love universal relation holds to 0.13% across twelve (m,as,ζ) models, and the ζ=0 and ζ=1 sequences sit on opposite sides of the master curve by a consistent, non-random offset. Applied without modification to realistic nuclear matter (SLy, APR4), the same solver reproduces published maximum masses to within 1%; applied to self-bound MIT-bag quark matter it gives the expected mass--radius shape; and once extended to a two-fluid baryon-plus-dark-matter formalism, it shows that the maximum mass of a hybrid star is not a monotonic function of the central dark-matter fraction. Pooling I-Love sequences across nuclear, hybrid, and BEC dark-star models, we find they collapse onto a single curve to within about 5%, while self-bound quark stars sit far off it, departing by up to 90%.
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BibTeX
@misc{ilyas2026parameter,
title = {{Parameter Space, Realistic Matter, and Universal Relations in Bose--Einstein Condensate Dark Stars}},
author = {M. Ilyas},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.01646},
eprint = {2609.01646},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.01646},
}
RIS
TY - UNPB
TI - Parameter Space, Realistic Matter, and Universal Relations in Bose--Einstein Condensate Dark Stars
AU - M. Ilyas
PY - 2026
DA - 2026/09/01
PB - arXiv
DO - 10.48550/arxiv.2609.01646
UR - https://arxiv.org/abs/2609.01646
AB - We study slowly rotating Bose--Einstein condensate (BEC) dark stars by solving the Tolman--Oppenheimer--Volkoff, Hartle dipole, and Postnikov--Hinderer equations together for a polytropic equation of state with a Lee--Huang--Yang correction of strength ζ~\citep{Panotopoulos2026}. A continuous scan of ζ from 0 to 1.5 shows the mean-field-to-corrected transition is smooth, with no hidden structure at intermediate values. Scanning the underlying boson parameters (m,a_s) more broadly, we find that a 2 M_⊙ maximum-mass bound and a GW170817-like tidal bound Λ_1.4≲800 cannot be satisfied simultaneously anywhere in this equation-of-state class. The I-Love universal relation holds to 0.13% across twelve (m,a_s,ζ) models, and the ζ=0 and ζ=1 sequences sit on opposite sides of the master curve by a consistent, non-random offset. Applied without modification to realistic nuclear matter (SLy, APR4), the same solver reproduces published maximum masses to within 1%; applied to self-bound MIT-bag quark matter it gives the expected mass--radius shape; and once extended to a two-fluid baryon-plus-dark-matter formalism, it shows that the maximum mass of a hybrid star is not a monotonic function of the central dark-matter fraction. Pooling I-Love sequences across nuclear, hybrid, and BEC dark-star models, we find they collapse onto a single curve to within about 5%, while self-bound quark stars sit far off it, departing by up to 90%.
ER -