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・ Photon entanglement
・ Photon epoch
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Photon surface
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Photon surface : ウィキペディア英語版
Photon surface

Photon sphere (''definition''〔K.S. Virbhadra and G. F.R. Ellis, Schwarzschild black hole lensing, Phys. Rev. D62, 084003 (2000); K.S. Virbhadra and G. F.R. Ellis, Gravitational lensing by naked singularities, Phys. Rev. D65, 103004 (2002).〕):

A photon sphere of a static spherically symmetric metric is a timelike hypersurface \ if the deflection angle of a light ray with the closest distance of approach r_o diverges as r_o \rightarrow r_.
For a general static spherically symmetric metric
g = - \beta\left(r\right) dt^2 - \alpha(r) dr^2 - \sigma(r) r^2 (d\theta^2 + \sin^2\theta d\phi^2),
the photon sphere equation is:
2\sigma(r) \beta + r \frac \beta(r) - r \frac \sigma(r) = 0.
The concept of a photon sphere in a static spherically metric was generalized to a photon surface of any metric.
Photon surface (''definition''〔Clarissa-Marie Claudel, K.S. Virbhadra, and G.F.R. Ellis, The geometry of photon surfaces, J. Math. Phys. 42, 818-838 (2001).〕) :

A photon surface of (M,g) is an immersed, nowhere spacelike hypersurface S of (M, g) such that, for every point p∈S and every null vector k∈''T''pS, there exists a null geodesic :(-ε,ε)→M of (M,g) such that {\dot{\gamma}}(0)=k, |γ|⊂S.
Both definitions give the same result for a general static spherically symmetric metric.〔See in ().〕
Theorem:〔See in ().〕

Subject to an energy condition, a black hole in any spherically symmetric spacetime must be surrounded by a photon sphere. Conversely, subject to an energy condition, any photon sphere must cover more than a certain amount of matter, a black hole, or a naked singularity.
==References==

Category:General relativity

抄文引用元・出典: フリー百科事典『 ウィキペディア(Wikipedia)
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