Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-percent level.
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Plane-parallel analysis finds MRI operates in solids only when magnetic tension exceeds shear modulus, requiring spin frequencies ≳300 Hz for crust amplification in neutron-star mergers.
citing papers explorer
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The crust of dark-matter admixed neutron stars: bulk properties and torsional oscillations
Dark matter admixed neutron stars show up to 12% thinner crusts and higher torsional oscillation frequencies than pure neutron stars when dark matter forms a core, with analytical formulas matching numerics at sub-percent level.
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Magneto-rotational instabilities in solids: application to neutron-star crusts
Plane-parallel analysis finds MRI operates in solids only when magnetic tension exceeds shear modulus, requiring spin frequencies ≳300 Hz for crust amplification in neutron-star mergers.