Hybrid neutron stars with slow hadron-quark conversion can remain radially stable beyond the maximum mass, and the extent of this stable branch depends on the quark-hadron energy density jump and quark matter stiffness.
Glendenning,Compact stars: Nuclear physics, particle physics, and general relativity (1997)
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Radial Oscillations in Hybrid Stars with Slow Quark Phase Transition
Hybrid neutron stars with slow hadron-quark conversion can remain radially stable beyond the maximum mass, and the extent of this stable branch depends on the quark-hadron energy density jump and quark matter stiffness.