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Recent progress in deriving the Page curve for unitary black hole evaporation is a significant step towards finding both a resolution to the information paradox and a more general understanding of unitarity in quantum gravity. [21] Many researchers consider deriving the Page curve as synonymous with solving the black hole information paradox.
Outside of the black hole's event horizon, semi-classical field equations remain valid. A black hole is a quantum system with discrete energy levels, as viewed by a distant observer. A free falling observer encounters nothing unique or strange; passing the event horizon is not marked by observable phenomena intrinsic to the horizon itself.
Stephen Hawking’s suggestion that black holes “leak” radiation left physicists with a problem they have been attempting to solve for 51 years.
The simplest models of black hole evaporation lead to the black hole information paradox. The information content of a black hole appears to be lost when it dissipates, as under these models the Hawking radiation is random (it has no relation to the original information).
A black hole with the mass of a car would have a diameter of about 10 −24 m and take a nanosecond to evaporate, during which time it would briefly have a luminosity of more than 200 times that of the Sun. Lower-mass black holes are expected to evaporate even faster; for example, a black hole of mass 1 TeV/c 2 would take less than 10 −88 ...
The Thorne–Hawking–Preskill bet was a public bet on the outcome of the black hole information paradox made in 1997 by physics theorists Kip Thorne and Stephen Hawking on the one side, and John Preskill on the other, according to the document they signed 6 February 1997, [1] as shown in Hawking's 2001 book The Universe in a Nutshell.
Depending on the model, primordial black holes could have initial masses ranging from 10 −8 kg [17] (the so-called Planck relics) to more than thousands of solar masses. . However, primordial black holes originally having masses lower than 10 11 kg would not have survived to the present due to Hawking radiation, which causes complete evaporation in a time much shorter than the age of the ...
It was previously thought that Hawking evaporation set the lower bound of primordial black holes to be 10 12 kg, but nonsingular black holes, which form remnants and do not evaporate completely, lower this bound to the Planck mass, which is 10 −8 kg. Thus Planck mass nonsingular black holes formed primordially can comprise all of the dark ...