Vol. Science · Astronomy · Horizon
A non-rotating black hole has one length that sets the rest. The Schwarzschild radius is rs = 2GM/c². Light can circle, unstably, at the photon sphere, 1.5 rs. The innermost stable circular orbit for a massive particle is the ISCO, 3 rs. Slide the mass from one solar mass to ten billion. The drawing is in units of rs, so the circles keep their shape and the kilometers change. A second control places a hovering observer. That clock runs at √(1 − rs/r) compared with a clock far away. The stretch across a 2 m body at the horizon is 2GM L / r³. Hawking temperature and an evaporation time are order-of-magnitude figures. Newtonian escape speed reaches c at this same radius — the escape desk. A high-mass star’s rough end is the stellar lifetime desk. Curvature, named without these radii, is gravity. A wavelength shift from motion or expansion is redshift.
Schwarzschild geometry. Educational approximation. Real astrophysical black holes spin, so the spacetime is Kerr and the photon orbit and the ISCO move. Bardeen, Press, and Teukolsky 1972 put the photon orbit at 3M when the spin is zero, and at M (prograde) or 4M (retrograde) when the spin is maximal. Their zero-spin stability condition is r > 6M, which is 3 rs. This page holds the two orbits at 1.5 rs and 3 rs. It does not draw a disk, a jet, or a shadow. The 1 and 10 solar-mass buttons are computed anchors. Named masses are cited central values. Radii, the tide, and the temperature use the IAU nominal GM☉. Density and the evaporation time also divide by the CODATA value of G.
Horizon, photon sphere, ISCO · drag the observer
Units of rs. Mass changes the kilometers. This picture keeps its shape. At 1 M☉, rs is 2.953 km.
Presets · computed anchors and cited central masses
Mass from 1 to 10 billion solar masses.
Observer from 1.2 to 30 Schwarzschild radii, outside the horizon.
Spin, tides, and a cold glow
Kerr’s geometry has mass and spin. The photon orbit and the ISCO depend on that spin and on whether the orbit turns with the hole or against it. Bardeen, Press, and Teukolsky 1972 give the zero-spin photon orbit at 3M and the maximal-spin photon orbit at M or 4M. The zero-spin ISCO is 6M. This desk does not evaluate the Kerr formula, and it does not assign a spin to Cygnus X-1, Sagittarius A*, or M87*. The EHT 2022 comparison for Sagittarius A* disfavors a non-spinning hole. The mass on the button is still the GRAVITY central value, and the radii are still the non-spinning ones.
The tide is 2GM L / r³ at r = r_s, with L = 2 m. That is the Newtonian difference in acceleration across a body about two metres tall. At one solar mass it is about two billion g. At Sagittarius A* it is a small fraction of one g. At M87* it is tiny. “Spaghettified at the horizon” is a stellar-mass story. A static observer’s proper tidal field diverges as the horizon is approached. This page does not compute that divergence. A traveler who falls in crosses the horizon in finite proper time. The clock factor on this page is for someone trying to hover.
Hawking temperature is ħ c³ / (8 π G M k). It scales as 1/M. A solar-mass hole is far colder than the cosmic microwave background, so it would absorb that bath faster than it radiates. The evaporation row assumes nothing falls in. It uses the horizon area as a blackbody, A = 4π r_s², which integrates to t = 5120 π G² M³ / (ħ c⁴). Page 1976 counted greybodies and other massless species and got a different power. The number here is an order of magnitude, and it scales as M³.
Mean density is the mass divided by the volume of the horizon sphere. It is an accounting figure, and it scales as 1/M². The mass is not a uniform ball of material. At M87* that quotient sits below the density of water, 1000 kg/m³. The comparison with water is the classroom 1000 kg/m³, and the comparison in g uses the conventional standard gravity 9.80665 m/s².
Literacy · the numbers on the readout
Sources · the constants and the masses
Classroom Schwarzschild arithmetic. rs = 2GM/c² with the IAU 2015 nominal GM☉ and the exact speed of light. Photon sphere 1.5 rs. ISCO 3 rs. The clock factor is √(1 − rs/r). The horizon tide is 2GM L/r³ across 2 m. Hawking temperature uses ħ, c, k, and GM. The evaporation time is the horizon-area order of magnitude, in Julian years. Density uses 2022 CODATA G. Named masses are the cited central values. Real holes spin. Earthrise preview: NASA / Bill Anders (public domain).
Keep going
The speed
Newtonian escape is √(2GM/r). It equals c at r = 2GM/c². That desk stays with fact-sheet planets. This one starts at that radius.
The path
Mass, a mass–luminosity fit, and t ≈ 10 Gyr × M/L. The black-hole label there is NASA’s rough end for a heavy star.
The pull
Weight, Newton, and Einstein. The black-hole card there is a definition. The radii are here.
The shift
z = (λ_obs − λ_rest)/λ_rest. At z = 1 the relativistic β is 0.6. Gravitational redshift is the clock factor on this page, written as z = 1/f − 1.
Letters
OBAFGKM and the life-path cartoons. The high-mass path is the one that can leave a hole.
Neighborhood
The nominal Sun this desk starts from, and the rest of the astronomy desks.
A non-rotating hole. The drawing is in units of r_s, so every mass looks the same and the readout carries the kilometers. Real holes spin.
| Horizon | Filled disk. Radius 1, in units of r_s. |
|---|---|
| Photon sphere | Dashed circle at 1.5 r_s. |
| ISCO | Solid circle at 3 r_s. |
| Observer | The marker. Drag it, or use the observer slider. It stays outside the horizon, from 1.2 r_s to 30 r_s. |
| Scale | The frame fits the ISCO and the observer. Mass does not redraw the circles. It changes the kilometer note. |
| Presets | 1 M☉ and 10 M☉ are computed from the IAU nominal GM☉. Cygnus X-1, Sagittarius A*, and M87* place the cited central mass. The observer stays where you left it. |
|---|---|
| Mass | Logarithmic, from 1 to 10 billion solar masses. Typing or sliding leaves the preset. |
| Observer | Distance in Schwarzschild radii, from 1.2 to 30. The clock factor needs a static observer outside the horizon. |
| Diagram | Tap or drag to set the observer from the distance to the center. It does not change the mass. |
| r_s, photon, ISCO | 2GM/c², 1.5 r_s, and 3 r_s. Kilometers, or AU when that is the readable unit. |
|---|---|
| Mean density | Mass over the volume inside r_s. The water column uses 1000 kg/m³. |
| Clock factor | √(1 − r_s/r). At 10 r_s it is 0.9487. The sentence under the card turns that into a gravitational redshift. |
| Horizon tide | 2GM L / r³ at the horizon, L = 2 m, also in units of standard gravity 9.80665 m/s². |
| Hawking T | ħ c³ / (8 π k GM). Colder as the hole gets heavier. |
| Evaporation | 5120 π G² M³ / (ħ c⁴), in Julian years. Labeled an order of magnitude. |
| Diagram | The canvas takes focus. Left and Right nudge the observer. Shift is a coarser step. |
|---|---|
| Buttons | Enter or Space selects. The pressed button is aria-pressed. Targets are at least 44 pixels on a side. |
| This dialog | The question mark, or ?, opens it. Escape closes it. Tab stays inside until you close it. Click the dim page behind the card to close it. |