Shadows of Rotating Black Holes

Although a black hole is not visible, you can observe it nonetheless  it casts a shadow if it is in front of a bright background. Since the early 1970's (Bardeen 1973, Luminet 1979, Quien et al. 1995, Hollywood and Melia 1997, Falcke et al. 2000, Bromley et al. 2001) the apparent shapes of special black holes have been computed, de Vries (2000) plotted the shadows of general rotating and electrically charged black holes, in dependence on their angular momentum and charge. You can press the following button to let such shadow curves be drawn.
In the sequel you will find concise explanations about: How can these shadow curves be determined? What are the basic principles of the computations?
The key idea to compute the apparent shape of a general black hole relies on geometrical optics: an electromagnetic wave propagates approximately on a congruence of light rays perpendicular to the wave fronts. Now, according to general relativity, light rays are bended lines in a spacetime curved by existing masses.
However, the geometric optics approximation is valid only if the wavelength λ is small as compared to the typical radius of curvature in the considered spacetime region. For a black hole of solar mass, e.g., the socalled event radius r_{+} (the "rim" of the black hole) is about 1.5 km, that is the same magnitude as the radius of curvature close to it. Therefore, for medium wave radiation (with λ between 100 m and 1 km) originated close to its event horizon geometrical optics is not an admissible approximation, but for very high frequency it is, a fortiori for even shorter waves like infrared waves, light, or xrays.
For the center of our Milky Way, presumably a giant black hole of about 2.6 million solar masses, the radius of curvature is about 4 million km, i.e., the error of a measurement of a long wave source (λ about 10 km) close to the event horizon is about 1:400000.
If we put up with inaccuracy of geometric optics, we get aware of the world around us as an optical illusion. Since the light rays reaching an observer in infinity are curved, they appear to come from a totally different direction. To represent the apparent source location with respect to the projection plane of the observer the (x, y) coordinates are used, as explained in the following figure:
Fig. 1.
The (x,y) coordinates, indicating the apparent position of a
light ray with respect to the observer's projection plane
containing the center of the spacetime: x denotes the apparent
distance from the rotation axis, and y the projection of the
rotation axis itself (dashed line).
denotes the
angle of latitude (reaching from the north pole at
= 0
to the south pole at
= ).

Further analysis of the light rays in a general KerrNewman spacetime (a generalization of a rotating, electrically charged black hole) with a singularity shows the existence of photons which move on closed orbits (Bardeen 1973, Chandrasekhar 1983, de Vries 2000), i.e., on ellipses. Such orbits describe the limit of the innermost photon orbits coming from infinity and escaping back to infinity. (Here "infinity" means the asymptotically flat spacetime region far away from the black hole; yet already at a distance of 25 times the event radius, 25r_{+}, the radius of curvature is R = 125r_{+}, so the asymptotically flat regions are reached rather quickly.)
Thus for an observer at infinity, who sees the black hole in front of an illuminated background in the asymptotic flat region, the black hole casts a shadow which in the approximation of geometrical optics is given by the set of its closed photon orbits.
de Vries (2000) has analyzed the nonlinear system of differential equations governing closed photon orbits. He found that for a KerrNewman spacetime (that is a spacetime generalization of a black hole) with mass M angular momentum a and electrical charge Q, the apparent position of a photon moving on a closed orbit with radius r in the (x, y) reference frame of an asymptotic observer located in the angle of latitude is given by
x =  rD + rQ^{2}  M (r^{2}  a^{2}) 
a (rM) sin 
y^{2} =  4r^{2}D   ( x  a sin )^{2}. 
(rM)^{2} 
with D = r^{2}  2Mr + a^{2} + Q^{2}. For parameters satisfying the "cosmic censorship hypothesis" (Penrose 1979), prohibiting naked singularities, viz. M^{2} ≤ a^{2} + Q^{2} (de Vries and SchmidtKaler 2002), these formulas yield welldefined closed curves on the celestial sphere of the asymptotic observer, the black hole shadow curves. Please click the following button to let some shadow curves be drawn.
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© de Vries 2003 