2017-08-15

[public] 554K views, 17.4K likes, 579 dislikes audio only

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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–Volkoff_limit

Richard Pogge (Ohio State) on Neutron & White Dwarf Stars: http://www.astronomy.ohio-state.edu/~pogge/Ast162/Unit3/extreme.html

Richard Pogge on Star Formation: http://www.astronomy.ohio-state.edu/~pogge/Ast162/Unit2/starform.html

Richard Pogge on Black Holes

Differences between galaxies and galaxy clusters: https://www.newscientist.com/article/dn20026-when-is-a-group-of-stars-not-a-galaxy/

Introductory/review Paper on Neutron Stars: https://arxiv.org/pdf/1102.5735.pdf

White dwarf stars on hyperphysics: http://hyperphysics.phy-astr.gsu.edu/hbase/Astro/whdwar.html

Brown Dwarf: https://en.wikipedia.org/wiki/Brown_dwarf

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