Image of a black hole illuminated by a parabolic screen

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Abstract

A model of an illuminating black hole surface (“parabolic screen”) is proposed. This allows to avoid in a natural way the appearance of edge effects related with photons moving along the screen plane. The temperature distribution along the radius corresponds to the corresponding distribution for a relativistic disk (Novikov-Thorne disk). It is shown that the structure of the formed black hole shadow essentially differs from the case when the source of photons is a distant screen, since in the considered model the photons, subjected to strong gravitational lensing of the black hole, are emitted by the “backward” side of screen, which would not be visible in the absence of the black hole. In the thin screen approximation, shadow images are constructed for the Schwarzschild black hole in the cases when the angle between the symmetry axis of the illuminating screen and the direction to the observer is equal to 5, 30, 30 and 80 angular degrees, similar images for the Kerr black hole are constructed for the cases of 60 and 80 angular degrees.

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About the authors

E. V. Mikheeva

Astrospace Center of P. N. Lebedev Physical Institute of the Russian Academy of Sciences

Author for correspondence.
Email: helen@asc.rssi.ru
Russian Federation, Moscow

S. V. Repin

Astrospace Center of P. N. Lebedev Physical Institute of the Russian Academy of Sciences

Email: sergerepin1@gmail.com
Russian Federation, Moscow

V. N. Lukash

Astrospace Center of P. N. Lebedev Physical Institute of the Russian Academy of Sciences

Email: lukash@asc.rssi.ru
Russian Federation, Moscow

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2. Fig. 1. Schematic of the radiating screen in the vicinity of the black hole. The black hole is located at the origin of coordinates, the dark gray zone corresponds to the region of space limited by the orbits of photons in the minimum stable orbit for the case of a Schwarzschild black hole.

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3. Fig. 2. Shadow of a Schwarzschild black hole. The angle between the axis of symmetry of the screen and the direction to the observer is 5°.

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4. Fig. 3. Shadow of a Schwarzschild black hole. The angle between the axis of symmetry of the screen and the direction to the observer is 30°.

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5. Fig. 4. Shadow of a Schwarzschild black hole. The angle between the axis of symmetry of the screen and the direction to the observer is 60°.

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6. Fig. 5. Shadow of a Schwarzschild black hole. The angle between the axis of symmetry of the screen and the direction to the observer is 80°.

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7. Fig. 6. Shadow of the Kerr black hole. The angle between the axis of rotation of the black hole and the direction to the observer is 60°.

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8. Fig. 7. Shadow of the Kerr black hole. The angle between the axis of rotation of the black hole and the direction to the observer is 80°.

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