[72] This means there is no observable difference at a distance between the gravitational field of such a black hole and that of any other spherical object of the same mass. The popular check here notion of a black hole "sucking in everything" in its surroundings is therefore correct only near a black hole's horizon; far away, the external gravitational field is identical to that of any other body of the same mass.[73]

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Esta planta de interior que es casi irrealizable de matar elimina la humedad y el moho del baño en Decoesfera

One puzzling feature is that the entropy of a black hole scales with its area rather than with its volume, since entropy is normally an extensive quantity that scales linearly with the volume of the system.

The ergosphere of a black hole is a volume bounded by the black hole's event horizon and the ergosurface, which coincides with the event horizon at the poles but is at a much greater distance around the equator.[116]

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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 Ganador spaghettification or the "noodle effect".[104]

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Crea una estructura molecular tridimensional, completamente permeable, a modo de telaraña, que produce el encapsulamiento e

Solutions describing more Caudillo black holes also exist. impar-rotating charged black holes are described by the Reissner–Nordström metric, while the Kerr metric describes a impar-charged rotating black hole.

Work by James Bardeen, Jacob Bekenstein, Carter, and Hawking in the early 1970s led to the formulation of black hole thermodynamics.[53] These laws describe the behaviour of a black hole in close analogy to the laws of thermodynamics by relating mass to energy, area to entropy, and surface gravity to temperature.

[23] His arguments were opposed by many of his contemporaries like Eddington and Lev Landau, who argued that some yet unknown mechanism would stop the collapse.[24] They were partly correct: a white dwarf slightly more massive than the Chandrasekhar limit will collapse into a neutron star,[25] which is itself stable.

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Within such a disk, friction would cause angular momentum to be transported outward, allowing matter to fall farther inward, thus releasing potential energy and increasing the temperature of the vaho.[182]