Hawking radiation In 1975,
Stephen Hawking argued that, due to
quantum effects, black holes "evaporate" by a process now referred to as
Hawking radiation in which elementary particles (such as
photons,
electrons,
quarks and
gluons) are emitted. His calculations showed that the smaller the size of the black hole, the faster the evaporation rate, resulting in a sudden burst of particles as the micro black hole suddenly explodes. Any primordial black hole of sufficiently low mass will
evaporate to near the
Planck mass within the lifetime of the Universe. In this process, these small black holes radiate away matter. A rough picture of this is that pairs of
virtual particles emerge from the
vacuum near the
event horizon, with one member of a pair being captured, and the other escaping the vicinity of the black hole. The net result is the black hole loses mass (due to
conservation of energy). According to the formulae of
black hole thermodynamics, the more the black hole loses mass, the hotter it becomes, and the faster it evaporates, until it approaches the Planck mass. At this stage, a black hole would have a
Hawking temperature of (), which means an emitted Hawking particle would have an energy comparable to the mass of the black hole. Thus, a thermodynamic description breaks down. Such a micro black hole would also have an entropy of only 4
nats, approximately the minimum possible value. At this point then, the object can no longer be described as a classical black hole, and Hawking's calculations also break down. While Hawking radiation is sometimes questioned,
Leonard Susskind summarizes an expert perspective in his book
The Black Hole War: "Every so often, a physics paper will appear claiming that black holes don't evaporate. Such papers quickly disappear into the infinite junk heap of fringe ideas."
Conjectures for the final state Conjectures for the final fate of the black hole include total evaporation and production of a
Planck-mass-sized black hole remnant. Such Planck-mass black holes may in effect be stable objects if the quantized gaps between their allowed energy levels bar them from emitting Hawking particles or absorbing energy gravitationally like a classical black hole. In such case, they would be
weakly interacting massive particles; this could explain
dark matter. == Primordial black holes ==