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It is an example of quantum foam and is the gravitational analog of the virtual electron–positron pairs found in quantum electrodynamics. Theoretical arguments suggest that virtual black holes should have mass on the order of the Planck mass, lifetime around the Planck time, and occur with a number density of approximately one per Planck ...
The spin quantum number of an elementary particle, usually called just "spin", a constant with a value of n / 2 , where n is a non-negative integer Topics referred to by the same term This disambiguation page lists articles associated with the title Spin parameter .
A rotating black hole is a black hole that possesses angular momentum. In particular, it rotates about one of its axes of symmetry. All celestial objects – planets, stars , galaxies, black holes – spin. [1] [2] [3] The boundaries of a Kerr black hole relevant to astrophysics. Note that there are no physical "surfaces" as such.
Black hole greybody factors are functions of frequency and angular momentum that characterizes the deviation of the emission-spectrum of a black hole from a pure black-body spectrum. As a result of quantum effects, an isolated black hole emits radiation that, at the black-hole horizon, matches the radiation from a perfect black body. [ 1 ]
In black hole theory, the black hole membrane paradigm is a simplified model, useful for visualising and calculating the effects predicted by quantum mechanics for the exterior physics of black holes, without using quantum-mechanical principles or calculations.
Extremal black hole – black hole with the minimal possible mass that can be compatible with a given charge and angular momentum. Black hole electron – if there were a black hole with the same mass and charge as an electron, it would share many of the properties of the electron including the magnetic moment and Compton wavelength.
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.
This explains why the "particle numbers", which are defined in terms of the creation and annihilation operators, are different in both coordinates. The Rindler spacetime has a horizon, and locally any non-extremal black hole horizon is Rindler. So the Rindler spacetime gives the local properties of black holes and cosmological horizons.