What Stops White Dwarfs and Neutron Stars From Collapsing?

What stops white dwarfs and neutron stars from collapsing, once the fusion that supported them is gone? In this episode of The Sleeping Physicist, we explore degeneracy pressure, the exclusion principle, relativity, and the mass limits that decide whether a dead star becomes a white dwarf, a neutron star, or a black hole. Learn why white dwarfs can remain stable without burning anything, how electron degeneracy pressure resists gravity, why this pressure does not depend on temperature, and what the Chandrasekhar limit reveals about the ultimate mass a white dwarf can support. We also explore how collapsing matter undergoes electron capture, how neutron degeneracy pressure takes over, and why even neutron stars face a final limit described by the Tolman Oppenheimer Volkoff equation. Like the video if you enjoy calm, clear physics Subscribe for more science, space, and universe explanations Comment where you’re listening from or what physics topic you’d like next 00:00:00 Star That Shouldn't Exist 00:03:25 What Living Stars Do 00:07:32 Collapse Is Default 00:11:37 Electrons Under Compression 00:16:17 Exclusion As Pressure Source 00:21:07 The Fermi Gas 00:26:32 Fermi Energy And Pressure 00:32:07 White Dwarfs As Fermi Gas 00:35:26 Chandrasekhar Limit 00:37:38 Relativity Enters Compression 00:40:03 Ceiling Reached, Collapse Begins 00:42:41 Neutron Stars Born 00:45:12 Neutron Degeneracy Pressure 00:47:53 TOV Equation 00:50:59 TOV Limit Reached 00:53:41 Beyond All Pressure 00:56:24 Degeneracy Pressure Defined 00:58:35 What Pressure Really Is #WhiteDwarfs #NeutronStars #BlackHoles #DegeneracyPressure #Astrophysics #QuantumPhysics #Relativity #Cosmology #PhysicsExplained #TheSleepingPhysicist