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The Schwarzschild radius or the gravitational radius is a physical parameter in the Schwarzschild solution to Einstein's field equations that corresponds to the radius defining the event horizon of a Schwarzschild black hole. It is a characteristic radius associated with any quantity of mass.
1923 — George David Birkhoff proves that the Schwarzschild spacetime geometry is the unique spherically symmetric solution of the Einstein vacuum field equations 1931 — Subrahmanyan Chandrasekhar calculates, using special relativity, that a non-rotating body of electron-degenerate matter above a certain limiting mass (at 1.4 solar masses ...
Any such model requires that the Hubble radius of the observable universe be equal to its Schwarzschild radius, that is, the product of its mass and the Schwarzschild proportionality constant. This is indeed known to be nearly the case; at least one cosmologist, however, considers this close match to be a coincidence. [3]
Timeline of black hole physics – Timeline of black hole physics; John Michell – geologist who first proposed the idea "dark stars" in 1783 [3] Dark star; Pierre-Simon Laplace – early mathematical theorist (1796) of the idea of black holes [4] [5] Albert Einstein – in 1915, arrived at the theory of general relativity
1916 – Karl Schwarzschild publishes the Schwarzschild metric about a month after Einstein published his general theory of relativity. [60] [61] This was the first solution to the Einstein field equations other than the trivial flat space solution. [62] [63] [64] 1916 – Albert Einstein predicts gravitational waves. [65]
The Schwarzschild radius of an object is proportional to its mass. Theoretically, any amount of matter will become a black hole if compressed into a space that fits within its corresponding Schwarzschild radius. For the mass of the Sun, this radius is approximately 3 kilometers (1.9 miles); for Earth, it is
1915: Karl Schwarzschild: discovery of the Schwarzschild radius leading to the identification of black holes; 1918: Emmy Noether: Noether's theorem – conditions under which the conservation laws are valid; 1920: Arthur Eddington: Stellar nucleosynthesis
In the Schwarzschild coordinates, the Schwarzschild radius = is the radial coordinate of the event horizon = =. In the Kruskal–Szekeres coordinates the event horizon is given by =. Note that the metric is perfectly well defined and non-singular at the event horizon.