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Science Astronomy Atmosphere

Vol. Science · Astronomy · Horizon

Black holes
one radius

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.

Interactive · Mass, orbits, and a hovering clock

Horizon, photon sphere, ISCO · drag the observer

  • Horizon
  • Photon sphere
  • ISCO
  • 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

M☉
rs

Spin, tides, and a cold glow

The picture is Schwarzschild. The holes in the sky spin.

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

Schwarzschild radius
rs = 2GM/c². In geometric units the horizon is r = 2M, so M = rs/2. One nominal solar mass uses the IAU 2015 mass parameter GM☉ = 1.3271244 × 10²⁰ m³ s⁻² and c = 299792458 m/s. That product is 2.953 km. G does not appear separately, because the mass parameter is already GM.
Photon sphere
The unstable circular orbit for light, at 1.5 rs (3M) when the hole does not spin. A slight nudge and the ray falls in or escapes. The shadow a telescope might see is larger than this circle, because of light bending. This page draws the orbit, not the shadow.
ISCO
Innermost stable circular orbit. For Schwarzschild it is 3 rs (6M). Inside it, a circular orbit is unstable and a slight inward nudge becomes a plunge. Gas in a thin disk is often described as drifting in until it reaches this orbit. Spin moves the orbit.
Clock factor
√(1 − rs/r) is dτ/dt for a static observer, relative to proper time at infinity. At 10 rs it is √0.9 = 0.9487. The same factor is a gravitational redshift, z = 1/f − 1. The redshift desk uses z = (λobs − λrest)/λrest for motion and for cosmic expansion. That z is a different measurement.
Horizon tide
2GM L / r³ at r = rs, L = 2 m. Because rs scales with M, the tide scales as 1/M². The “g” column divides by 9.80665 m/s², the conventional standard gravity. It is a comparison, not a second measurement of the hole.
Mean density
M / (⁴⁄₃ π rs³), with M = GM☉ / G and G = 6.67430 × 10⁻¹¹ m³ kg⁻¹ s⁻², the 2022 CODATA central value. “× water” divides by 1000 kg/m³. The quotient falls as 1/M². It is not the density of any material at the horizon.
Hawking temperature and evaporation
T = ħ c³ / (8 π k GM). ħ = h/(2π), with h and k the exact SI constants. The lifetime row is t = 5120 π G² M³ / (ħ c⁴), reported in Julian years of 31,557,600 s. That coefficient is the horizon-area Stefan–Boltzmann estimate. It is an order of magnitude. A hole colder than the cosmic microwave background gains energy from that radiation while the bath is warmer than T.
1 and 10 solar masses
Computed. The Sun’s nominal mass parameter, and ten times it. NASA’s classroom split leaves a white dwarf below about 8 solar masses and a neutron star from about 8 to 20. Neither button is a claim that such a hole exists at that mass.
Cited holes
Cygnus X-1, 21.2 ± 2.2 M☉, Miller-Jones et al. 2021. Sagittarius A*, (4.297 ± 0.012) × 10⁶ M☉ statistical, systematics about 40,000 M☉, GRAVITY Collaboration 2022. M87*, 6.5 ± 0.2 (stat) ± 0.7 (sys) × 10⁹ M☉, EHT 2019 Paper VI. The readout uses the central value.

Sources · the constants and the masses

Cited, not invented

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

Escape

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

Stellar lifetime

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

Gravity

Weight, Newton, and Einstein. The black-hole card there is a definition. The radii are here.

The shift

Redshift

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

Stars

OBAFGKM and the life-path cartoons. The high-mass path is the one that can leave a hole.

Neighborhood

Solar map

The nominal Sun this desk starts from, and the rest of the astronomy desks.