Black Hole Hi Light

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Black Hole Hi Light

From Wikipedia, the free encyclopedia
Astronomical object that has a no-return boundary





G

μ
ν


+
Λ

g

μ
ν


=

κ


T

μ
ν




{\displaystyle G_{\mu \nu }+\Lambda g_{\mu \nu }={\kappa }T_{\mu \nu }}


Simple illustration of a non-spinning black hole
Artistic depiction of a black hole and its features
Far away from the black hole, a particle can move in any direction, as illustrated by the set of arrows. It is restricted only by the speed of light.
Closer to the black hole, spacetime starts to deform. There are more paths going towards the black hole than paths moving away. [Note 3]
Inside of the event horizon, all paths bring the particle closer to the centre of the black hole. It is no longer possible for the particle to escape.
The formula for the Bekenstein–Hawking entropy ( S ) of a black hole, which depends on the area of the black hole ( A ). The constants are the speed of light ( c ), the Boltzmann constant ( k ), Newton's constant ( G ), and the reduced Planck constant ( ħ ). In Planck units, this reduces to S = A / 4 .

^ The value of cJ/GM 2 can exceed 1 for objects other than black holes. The largest value known for a neutron star is ≤ 0.4, and commonly used equations of state would limit that value to < 0.7. [76]

^ The (outer) event horizon radius scales as:



M
+



M

2


−


(
J

/

M
)


2


−

Q

2




.


{\displaystyle M+{\sqrt {M^{2}-{(J/M)}^{2}-Q^{2}}}.}



^ The set of possible paths, or more accurately the future light cone containing all possible world lines (in this diagram the light cone is represented by the V-shaped region bounded by arrows representing light ray world lines), is tilted in this way in Eddington–Finkelstein coordinates (the diagram is a "cartoon" version of an Eddington–Finkelstein coordinate diagram), but in other coordinates the light cones are not tilted in this way, for example in Schwarzschild coordinates they simply narrow without tilting as one approaches the event horizon, and in Kruskal–Szekeres coordinates the light cones do not change shape or orientation at all. [79]

^ This is true only for four-dimensional spacetimes. In higher dimensions more complicated horizon topologies like a black ring are possible. [91] [92]

^ In particular, he assumed that all matter satisfies the weak energy condition .



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