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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Fuzzy dark matter with smooth cored halos provides the most consistent description of M31's rotation curve among scalar field models when paired with a two-bulge baryonic configuration.
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Self-gravitating quantum stars with a globally relevant Bohm potential
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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Testing Scalar Field Dark Matter models in M31 galaxy through the Rotation Curve analysis
Fuzzy dark matter with smooth cored halos provides the most consistent description of M31's rotation curve among scalar field models when paired with a two-bulge baryonic configuration.