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Visualizing circular motion around a Schwarzschild black hole
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View: Figures


Image of Fig. 1.
Fig. 1.

The observer moves on a circular orbit with radius around a Schwarzschild black hole. The torus has radii and . The bold solid line represents a typical light ray. The black hole horizon with radius is indicated by the dashed line.

Image of Fig. 2.
Fig. 2.

Screenshot of the torus application. The Milky Way background image is taken from ESO (Ref. 22). The left overlay shows the observer’s current position, the orientation of the local reference frame, and the viewing direction. The right overlay shows the tidal accelerations. For a bigger view of the overlays, see Fig. 17.

Image of Fig. 3.
Fig. 3.

The projection shows the complete sky at a glance. The distortions close to are due to the projection itself. In this inverse-color image, the white region corresponds to the black hole. The direction of motion is , .

Image of Fig. 4.
Fig. 4.

Cross section of a torus in the -plane with outer radius and inner radius .

Image of Fig. 5.
Fig. 5.

To obtain a real circular shape of the inner circle of the torus with respect to proper distance (solid line) or with respect to constant light travel time (dashed line), must be a function of . Here, , , and .

Image of Fig. 6.
Fig. 6.

Initial wave vector with respect to the local reference frame of the observer.

Image of Fig. 7.
Fig. 7.

Gamuts representing Planck spectra for temperatures from to . (a) Scaled to maximum luminance value for each temperature; (b) scaled to luminance value for temperature .

Image of Fig. 8.
Fig. 8.

Torus in flat Minkowski space for comparison with the later examples in curved space. The observer is either (a) at rest or (b) moves with half the speed of light. In both cases, the observer is currently located at . The torus has an outer radius .

Image of Fig. 9.
Fig. 9.

Different looks of the three torus definitions: Pseudo-Cartesian, length-scaled, and time-scaled (from left to right). The vertical field of view is 20°, and the observer is located at .

Image of Fig. 10.
Fig. 10.

Torus with , , and (from top to bottom). The observer moves with half the speed of light and the vertical field of view of its camera is 20°. The viewing direction is parallel to the direction of motion. On the left side of the top image, the torus appears to extend into an Einstein ring.

Image of Fig. 11.
Fig. 11.

Schematic depiction of geodesics for different . Only the -plane is shown. In each picture, only the one geodesic that reaches the observer tangential to the -direction is considered. Depending on , the light ray (solid line) that the observer (black dot) sees as coming from directly ahead originates from the outer part of the torus (, outer dotted circle) or from the inner part (, inner dotted circle). This increasing bending of light rays with decreasing leads to the apparent change in the direction of bending of the torus for .

Image of Fig. 12.
Fig. 12.

If the torus encompasses the photon orbit, geodesics originating from a point can either reach the observer directly or orbit the black hole one or several times . Therefore, the observer sees the point with the corresponding observation angles , , etc. The gray area marks all points with .

Image of Fig. 13.
Fig. 13.

Torus with as in Fig. 10 but with a vertical field of view of only 2°.

Image of Fig. 14.
Fig. 14.

Torus with . The observer moves with (from top to bottom) and is currently at . The scaled proper times for one complete orbit are . The center of this projection is the direction of motion. (a) The spectrum scaled to -luminance. (b) The spectrum scaled to maximum luminance.

Image of Fig. 15.
Fig. 15.

Parallel-transport of the frame vector on the innermost stable circular timelike geodesic with (see also Ref. 29); and correspond to the natural local tetrad at that position.

Image of Fig. 16.
Fig. 16.

Geodesic precession for an observer on the timelike circular geodesic with and . The observer’s current position is (from top to bottom). The white disk represents the black hole. The colors are inverted in this projection to enhance the visual impression.

Image of Fig. 17.
Fig. 17.

(a) The orientation overlay shows the and frame vectors and the viewing direction of the moving observer. (b) The tidal accelerations overlay shows the direction and strengths of the tidal accelerations with respect to the observer’s reference frame. The central thick line indicates the direction to the black hole.

Image of Fig. 18.
Fig. 18.

Tidal acceleration for motion on the last stable timelike circular orbit with and . The central thick arrow shows the direction to the black hole.


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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: Visualizing circular motion around a Schwarzschild black hole