Supermassive black holes of millions of solar masses (M☉) may form by absorbing other stars and merging with other black holes, or via direct collapse of gas clouds. There is consensus that supermassive black holes exist in the centres of most galaxies.
Because a black hole eventually achieves a stable state with only three parameters, there is no way to avoid losing information about the initial conditions: the gravitational and electric fields of a black hole give very little information about what went in.
The Hawking radiation for an astrophysical black hole is predicted to be very weak and would thus be exceedingly difficult to detect from Earth. A possible exception, however, is the burst of gamma rays emitted in the last stage of the evaporation of primordial black holes.
If a black hole is very small, the radiation effects are expected to become very strong. 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/c2 would take less than 10−88 seconds to evaporate completely.
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[103] When they reach the singularity, they are crushed to infinite density and their mass is added to the total of the black hole. Before that happens, they will have been torn apart by the growing tidal forces in a process sometimes referred to Campeón spaghettification or the "noodle effect".[104]
To a distant observer, clocks near a black hole would appear to tick more slowly than those farther away from the black hole.[87] Due to this effect, known Ganador gravitational time dilation, an object falling into a black hole appears to slow Triunfador it approaches the event horizon, taking an infinite amount of time to reach it.
Esta "pintura" distinto promete descender la temperatura 10 ºC y que ahorremos en aerofagia acondicionado: Campeóní funciona
One attempt to resolve the black hole information paradox is known Figura black hole complementarity. In 2012, the "firewall paradox" was introduced with the goal of demonstrating that black hole complementarity fails to solve the information paradox. According to quantum field theory in curved spacetime, a single emission of Hawking radiation involves two mutually entangled particles. The outgoing particle escapes and is emitted Campeón a quantum of Hawking radiation; the infalling particle is swallowed by the black hole.
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On the other hand, indestructible observers falling into a black hole do not notice any of these effects Ganador they cross the event horizon. According to their own clocks, which appear to them to tick normally, they cross the event horizon after a finite time without noting any singular behaviour; in classical Militar relativity, it is impossible to determine the location of the event horizon from Particular observations, due to Einstein's equivalence principle.[91][92]