Latimer showed that the equation of state for one form of these objects is soft at low density and stiff at high density.
A pair of equations governing these objects has a solution named for Buchdahl. Latimer showed that the equation of state for one form of these objects is soft at low density and stiff at high density. These objects exhibition a phase transition from a spaghetti phase to a Swiss cheese phase when moving towards the core. Gamow and Scheonberg postulated a mechanism by which these stars would emit a neutrino to cool, known as the Urca process. These objects are postulated to have an outer core that consists of a Fermi liquid, while their core composition is unknown. The fact that their crusts are very stiff means that when these objects slow their rotation, the crust quickly adjusts in a starquake. The upper limit of these object's mass is postulated to be between 1.5 to 2 solar masses, a value known as the Tolman-Oppenheimer-Volkoff limit. They form when the core of a star collapses during a supernova. For 10 points, name these dense stars made of a namesake neutral particle
A pair of equations governing these objects has a solution named for Buchdahl.
{Neutron} Stars