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This video is about the differences between the corpses or final degenerate dense star forms that dead stars take: black holes, neutron stars, and white dwarfs. The main distinguishing features between them are the mass cutoffs (Chandrasekhar limit and Tolman-Oppenheimer-Volkoff Limit), the matter that makes them up (electrons, protons, neutrons, singularity?), and what holds them up against gravity – not thermal pressure from nuclear fusion like in a star like the sun, but electron or neutron degeneracy pressure (fermi pressure/pauli exclusion principle), and the strong nuclear force, and… nothing (in the case of a black hole).
REFERENCES:
Chandrasekhar Limit:
Tolman-Oppenheimer-Volkoff Limit:
Richard Pogge (Ohio State) on Neutron & White Dwarf Stars:
Richard Pogge on Star Formation:
Richard Pogge on Black Holes
Differences between galaxies and galaxy clusters:
Introductory/review Paper on Neutron Stars:
White dwarf stars on hyperphysics:
Brown Dwarf:
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Minute Physics provides an energetic and entertaining view of old and new problems in physics — all in a minute!
Created by Henry Reich
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