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On the Size of Rotating Black Holes
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Recently a sequence of inequalities relating the black hole horizon, photon sphere, shadow were proposed for spherically symmetric and static black holes, providing the upper bound for given mass. In this paper, we extend the discussion to include rotating black holes. When viewed from the north pole direction, the shadow remains a round disk, but the image is skewed when viewed from the equatorial plane. After properly implementing the ``size'' parameters for the rotating black holes, we verify that the sequence of inequalities remain valid for a variety of solutions, including Kerr, Kerr-Newman, Kerr-Sen and Kerr-Cveti\v c-Youm black holes. The upshot is that rotation makes both the actual and apparent sizes of a black hole smaller.
Forward citations
Cited by 2 Pith papers
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Bounds on the radius of outermost photon sphere and black hole shadow in $n$-dimensional Einstein gravity
Proves model-independent lower bound r_sh ≥ ((n-1)/2)^{1/(n-3)} sqrt((n-1)/(n-3)) r_H under WEC and upper bound r_sh ≤ sqrt((n-1)/(n-3)) [(n-1)M]^{1/(n-3)} under WEC+SEC+decay for nD black holes.
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The existence and upper bound for stable photon spheres in static spherically symmetric black holes
For static spherical black holes with monotone m(r)/r^3, every stable photon sphere obeys r < 6M.
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