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in the SP limit, is a noteworthy 14 feature, for it implies that a single microphysical paramet er, /u1D45A1, determines the equilibrium once the total mass is speci- fied, distinguishing these configurations from phenomenolo gical models w · 2025 · DOI 10.54499/uid/prr/00099/2025

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Self-gravitating quantum stars with a globally relevant Bohm potential

hep-th · 2026-05-31 · conditional · novelty 6.0

The equilibrium radius of self-gravitating dark fermion stars is determined by the fermion mass once the total mass is given, with the Bohm potential supplying outward pressure for heavier species and inward tension for lighter ones.

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  • Self-gravitating quantum stars with a globally relevant Bohm potential hep-th · 2026-05-31 · conditional · none · ref 16

    The equilibrium radius of self-gravitating dark fermion stars is determined by the fermion mass once the total mass is given, with the Bohm potential supplying outward pressure for heavier species and inward tension for lighter ones.