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Classically, black holes are black.

Quantum mechanically, black holes radiate, with a radiation known as Hawking radiation, after the British physicist Stephen Hawking who first proposed it.

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Hawking radiation has a blackbody (Planck) spectrum with a temperature T given by

kT = hbar g / (2 pi c) = hbar c / (4 pi r_s)

where k is Boltzmann's constant, hbar = h / (2 pi) is Planck's constant divided by 2 pi, and g = G M / r_s² is the surface gravity at the horizon, the Schwarzschild radius r_s, of the black hole of mass M. Numerically, the Hawking temperature is T = 4 × 10^-20 g Kelvin if the gravitational acceleration g is measured in Earth gravities (gees).

The Hawking luminosity L of the black hole is given by the usual Stefan-Boltzmann blackbody formula

L = A sigma T⁴

where A = 4 pi r_s² is the surface area of the black hole, and sigma = pi² k⁴ / (60 c² hbar³) is the Stefan-Boltzmann constant. If the Hawking temperature exceeds the rest mass energy of a particle type, then the black hole radiates particles and antiparticles of that type, in addition to photons, and the Hawking luminosity of the black hole rises to

L = A (n_eff / 2) sigma T⁴

where n_eff is the effective number of relativistic particle types, including the two helicity types (polarizations) of the photon.