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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: https://en.wikipedia.org/wiki/Chandrasekhar_limit
Tolman-Oppenheimer-Volkoff Limit: https://en.wikipedia.org/wiki/....Tolman–Oppenheimer–V
Richard Pogge (Ohio State) on Neutron & White Dwarf Stars: http://www.astronomy.ohio-stat....e.edu/~pogge/Ast162/
Richard Pogge on Star Formation: http://www.astronomy.ohio-stat....e.edu/~pogge/Ast162/
Richard Pogge on Black Holes
Differences between galaxies and galaxy clusters: https://www.newscientist.com/a....rticle/dn20026-when-
Introductory/review Paper on Neutron Stars: https://arxiv.org/pdf/1102.5735.pdf
White dwarf stars on hyperphysics: http://hyperphysics.phy-astr.g....su.edu/hbase/Astro/w
Brown Dwarf: https://en.wikipedia.org/wiki/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