A photon sphere[1] or photon circle[2] is an area or region of space where gravity is so strong that photons are forced to travel in orbits. (It is sometimes called the last photon orbit.)[3] The radius of the photon sphere, which is also the lower bound for any stable orbit, is, for a Schwarzschild black hole:

\( {\displaystyle r={\frac {3GM}{c^{2}}}={\frac {3r_{\rm {s}}}{2}}} \)

where G is the gravitational constant, M is the black hole mass, and c is the speed of light in vacuum and rs is the Schwarzschild radius (the radius of the event horizon) - see below for a derivation of this result.

This equation entails that photon spheres can only exist in the space surrounding an extremely compact object (a black hole or possibly an "ultracompact" neutron star[4]).

The photon sphere is located farther from the center of a black hole than the event horizon. Within a photon sphere, it is possible to imagine a photon that's emitted from the back of one's head, orbiting the black hole, only then to be intercepted by the person's eyes, allowing one to see the back of the head. For non-rotating black holes, the photon sphere is a sphere of radius 3/2 rs. There are no stable free fall orbits that exist within or cross the photon sphere. Any free fall orbit that crosses it from the outside spirals into the black hole. Any orbit that crosses it from the inside escapes to infinity or falls back in and spirals into the black hole. No unaccelerated orbit with a semi-major axis less than this distance is possible, but within the photon sphere, a constant acceleration will allow a spacecraft or probe to hover above the event horizon.

Another property of the photon sphere is centrifugal force (note: not centripetal) reversal.[5] Outside the photon sphere, the faster one orbits the greater the outward force one feels. Centrifugal force falls to zero at the photon sphere, including non-freefall orbits at any speed, i.e. you weigh the same no matter how fast you orbit, and becomes negative inside it. Inside the photon sphere the faster you orbit the greater your felt weight or inward force. This has serious ramifications for the fluid dynamics of inward fluid flow.

A rotating black hole has two photon spheres. As a black hole rotates, it drags space with it. The photon sphere that is closer to the black hole is moving in the same direction as the rotation, whereas the photon sphere further away is moving against it. The greater the angular velocity of the rotation of a black hole, the greater the distance between the two photon spheres. Since the black hole has an axis of rotation, this only holds true if approaching the black hole in the direction of the equator. If approaching at a different angle, such as one from the poles of the black hole to the equator, there is only one photon sphere. This is because approaching at this angle the possibility of traveling with or against the rotation does not exist.

Derivation for a Schwarzschild black hole

Since a Schwarzschild black hole has spherical symmetry, all possible axes for a circular photon orbit are equivalent, and all circular orbits have the same radius.

This derivation involves using the Schwarzschild metric, given by:

\( {\displaystyle ds^{2}=\left(1-{\frac {r_{\rm {s}}}{r}}\right)c^{2}dt^{2}-\left(1-{\frac {r_{\rm {s}}}{r}}\right)^{-1}dr^{2}-r^{2}({\textrm {sin}}^{2}\theta d\phi ^{2}+d\theta ^{2})} \)

For a photon traveling at a constant radius r (i.e. in the Φ-coordinate direction), \( {\displaystyle dr=0}\) . Since it is a photon \( {\displaystyle ds=0} \) (a "light-like interval"). We can always rotate the coordinate system such that \( \theta \) is constant, \( {\displaystyle d\theta =0} \) (i.e., \( \theta = \frac{\pi}{2}) \) .

Setting ds, dr and dθ to zero, we have:

\( {\displaystyle \left(1-{\frac {r_{\rm {s}}}{r}}\right)c^{2}dt^{2}=r^{2}{\textrm {sin}}^{2}\theta d\phi ^{2}} \)

Re-arranging gives:

\( {\displaystyle {\frac {d\phi }{dt}}={\frac {c}{r{\textrm {sin}}\theta }}{\sqrt {1-{\frac {r_{\rm {s}}}{r}}}}}\)

To proceed we need the relation d ϕ d t {\displaystyle {\frac {d\phi }{dt}}} \frac{d\phi}{dt} . To find it, we use the radial geodesic equation

\( \frac{d^2r}{d\tau^2}+\Gamma^{r}_{\mu\nu}u^{\mu}u^{\nu}=0.

Non vanishing \( \Gamma \) -connection coefficients are \( {\displaystyle \Gamma _{tt}^{r}={\frac {c^{2}BB^{\prime }}{2}},\;\Gamma _{rr}^{r}=-{\frac {B^{-1}B^{\prime }}{2}},\;\Gamma _{\theta \theta }^{r}=-rB,\;\Gamma _{\phi \phi }^{r}=-Br\sin ^{2}\theta } \) , where \( {\displaystyle B^{\prime }={\frac {dB}{dr}},B=1-{\frac {r_{\rm {s}}}{r}}}. \)

We treat photon radial geodesics with constant r and \( \theta \) , therefore

\( \; \frac{d^2r}{d\tau^2}, \; \frac{d\theta}{d\tau}=0 .\)

Substituting it all into the radial geodesic equation (the geodesic equation with the radial coordinate as the dependent variable), we obtain

\( {\displaystyle \left({\frac {d\phi }{dt}}\right)^{2}={\frac {c^{2}r_{\rm {s}}}{2r^{3}\sin ^{2}\theta }}} \)

Comparing it with what was obtained previously, we have:

\( {\displaystyle c{\sqrt {\frac {r_{\rm {s}}}{2r}}}=c{\sqrt {1-{\frac {r_{\rm {s}}}{r}}}}}\)

where we have inserted \( \theta = \frac{\pi}{2} \) radians (imagine that the central mass, about which the photon is orbiting, is located at the centre of the coordinate axes. Then, as the photon is travelling along the \( \phi \) -coordinate line, for the mass to be located directly in the centre of the photon's orbit, we must have \( \theta = \frac{\pi}{2} \) radians).

Hence, rearranging this final expression gives:

\( {\displaystyle r={\frac {3}{2}}r_{\rm {s}}} \)\)

which is the result we set out to prove.
Photon orbits around a Kerr black hole
Views from the side (l) and from above a pole (r). A rotating black hole has 9 radii between which light can orbit on a constant r-coordinate. In this animation, all photon-orbits for a=M are shown. Click to animate.

In contrast to a Schwarzschild black hole, a Kerr (spinning) black hole does not have spherical symmetry, but only an axis of symmetry, which has profound consequences for the photon orbits, see e.g. Cramer [2] for details and simulations of photon orbits and photon circles. A circular orbit can only exist in the equatorial plane, and there are two of them (prograde and retrograde), with different Boyer–Lindquist-radii,

\( {\textstyle r_{\pm }^{\circ }=r_{\rm {s}}\ \left[1+\cos \left({\frac {2}{3}}\cos ^{-1}\left({\frac {\pm |a|}{M}}\right)\right)\right],}\)

where \( {\displaystyle a=J/M} \) is the angular momentum per unit mass of the black hole.[6] There exist other constant coordinate-radius orbits, but they have more complicated paths which oscillate in latitude about the equator.[6]

General Relativity: An Introduction for Physicists

Bennett, Jay (April 10, 2019). "Astronomers Capture First-Ever Image of a Supermassive Black Hole". Smithsonian Institution. Retrieved April 15, 2019.
Cramer, Claes R (1997). "Using the Uncharged Kerr Black Hole as a Gravitational Mirror". General Relativity and Gravitation. 29 (4): 445–454. arXiv:gr-qc/9510053. Bibcode:1997GReGr..29..445C. doi:10.1023/A:1018878515046. S2CID 9517046.
"What the Sight of a Black Hole Means to a Black Hole Physicist", Quanta Magazine, 10 April 2019: "a region defined by the location closest to the black hole where a beam of light could orbit on a circle, known as the “last photon orbit”."
Properties of ultracompact neutron stars
Abramowicz, Marek (1990). "Centrifugal-force reversal near a Schwarzschild black hole". Monthly Notices of the Royal Astronomical Society. 245: 720. Bibcode:1990MNRAS.245..720A.

Teo, Edward (2003). "Spherical Photon Orbits Around a Kerr Black Hole" (PDF). General Relativity and Gravitation. 35 (11): 1909–1926. Bibcode:2003GReGr..35.1909T. doi:10.1023/A:1026286607562. ISSN 0001-7701. S2CID 117097507.

External links

Step by Step into a Black Hole
Virtual Trips to Black Holes and Neutron Stars
Guide to Black Holes
Spherical Photon Orbits Around a Kerr Black Hole


Black holes

Schwarzschild Rotating Charged Virtual Kugelblitz Primordial Planck particle


Extremal Electron Stellar
Microquasar Intermediate-mass Supermassive
Active galactic nucleus Quasar Blazar


Stellar evolution Gravitational collapse Neutron star
Related links Tolman–Oppenheimer–Volkoff limit White dwarf
Related links Supernova
Related links Hypernova Gamma-ray burst Binary black hole


Gravitational singularity
Ring singularity Theorems Event horizon Photon sphere Innermost stable circular orbit Ergosphere
Penrose process Blandford–Znajek process Accretion disk Hawking radiation Gravitational lens Bondi accretion M–sigma relation Quasi-periodic oscillation Thermodynamics
Immirzi parameter Schwarzschild radius Spaghettification


Black hole complementarity Information paradox Cosmic censorship ER=EPR Final parsec problem Firewall (physics) Holographic principle No-hair theorem


Schwarzschild (Derivation) Kerr Reissner–Nordström Kerr–Newman Hayward


Nonsingular black hole models Black star Dark star Dark-energy star Gravastar Magnetospheric eternally collapsing object Planck star Q star Fuzzball


Optical black hole Sonic black hole


Black holes Most massive Nearest Quasars Microquasars


Black Hole Initiative Black hole starship Compact star Exotic star
Quark star Preon star Gamma-ray burst progenitors Gravity well Hypercompact stellar system Membrane paradigm Naked singularity Quasi-star Rossi X-ray Timing Explorer Timeline of black hole physics White hole Wormhole

Physics Encyclopedia



Hellenica World - Scientific Library

Retrieved from ""
All text is available under the terms of the GNU Free Documentation License