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The observer-dependent shadow of the Kerr black hole
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Motivated by inclination of the Earth's orbit that is not located at galactic plane for observing the shadow of Sgr A*, we consider the black hole shadow for arbitrary inclinations and different velocities of observers. A surprising finding of the study is that rotation axis of a black hole might not be extracted from its shadow, since the ways of the shadow getting distorted depend not only on the spin of the black hole, but also velocities of observers. Namely, appearance of the shadow could be rotated by an angle in observers' celestial sphere due to the observer in motion. In order to further confirm this result, a formalism is presented for calculating the shadow in terms of the velocity perturbations. Besides, we also consider the Earth's orbit for the shadow of Sgr A* by making use of this formalism.
Forward citations
Cited by 2 Pith papers
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Critical Behavior of Photon Rings in Kerr-Bertotti-Robinson Spacetime
For a magnetized Kerr-Bertotti-Robinson black hole, the photon-ring parameters gamma, delta, and tau all decrease compared with the unmagnetized Kerr case, weakening the self-similar stacking of higher-order images.
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Optical Characteristics of the Kerr-Bertotti-Robinson Black Hole
For the Kerr-Bertotti-Robinson black hole, the magnetic field mainly enlarges the shadow and Einstein ring while rotation mainly distorts the shadow shape, and current M87* and Sgr A* data give only weak bounds on the field.
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