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Matches in DBpedia 2015-10 for { ?s ?p "Indeed, these uncertainty relations can be obtained on the basis of Einstein's equations where is the Einstein tensor, which combines the Ricci tensor, the scalar curvature and the metric tensor, is the cosmological constant, а energy-momentum tensor of matter, is the irrational number originally introduced as the ratio of the circumference of a circle to it's diameter, is the speed of light, — Newton's gravitational constant. In the derivation of his equations, Einstein suggested that physical space-time is Riemannian, ie curved. A small domain of it is approximately flat space-time. For any tensor field value we may call a tensor density, where - determinant of the metric tensor . The integral is a tensor if the domain of integration is small. It is not a tensor if the domain of integration is not small, because it then consists of a sum of tensors located at different points and it does not transform in any simple way under a transformation of coordinates. Here we consider only small domains. This is also true for the integration over the three-dimensional hypersurface . Thus, Einstein's equations for small space-time domain can be integrated by the three-dimensional hypersurface . Have : Since integrable space-time domain is small, we obtain the tensor equation where is the 4-momentum, is the radius of curvature domain. The resulting tensor equation can be rewritten in another form. Since then : where is the Schwarzschild radius, is the 4-speed, is the gravitational mass. This record reveals the physical meaning of . In a small area of space-time is almost flat and this equation can be written in the operator form : Then commutator operators and is : From here follow the specified uncertainty relations Substituting the values of and and cutting right and left of the same symbols, we obtain the Heisenberg uncertainty principle : In the particular case of a static spherically symmetric field and static distribution of matter and have remained : where is the Schwarzschild radius, is the radial coordinate. Last uncertainty relation allows make us some estimates of the equations of general relativity at the Planck scale. For example, the equation for the invariant interval в in the Schwarzschild solution has the form : Substitute according to the uncertainty relations . We obtain : It is seen that at the Planck scale space-time metric is bounded below by the Planck length, and on this scale, there are real and virtual Planckian black holes. Similar estimates can be made in other equations of general relativity. For example, analysis of the Hamilton-Jacobi equation for a centrally symmetric gravitational field in spaces of different dimensions indicates a preference for three-dimensional space for the emergence of virtual black holes . Prescribed above uncertainty relation valid for strong gravitational fields, as in any sufficiently small domain of a strong field space-time is essentially flat."@en }

• Virtual_black_hole content "Indeed, these uncertainty relations can be obtained on the basis of Einstein's equations where is the Einstein tensor, which combines the Ricci tensor, the scalar curvature and the metric tensor, is the cosmological constant, а energy-momentum tensor of matter, is the irrational number originally introduced as the ratio of the circumference of a circle to it's diameter, is the speed of light, — Newton's gravitational constant. In the derivation of his equations, Einstein suggested that physical space-time is Riemannian, ie curved. A small domain of it is approximately flat space-time. For any tensor field value we may call a tensor density, where - determinant of the metric tensor . The integral is a tensor if the domain of integration is small. It is not a tensor if the domain of integration is not small, because it then consists of a sum of tensors located at different points and it does not transform in any simple way under a transformation of coordinates. Here we consider only small domains. This is also true for the integration over the three-dimensional hypersurface . Thus, Einstein's equations for small space-time domain can be integrated by the three-dimensional hypersurface . Have : Since integrable space-time domain is small, we obtain the tensor equation where is the 4-momentum, is the radius of curvature domain. The resulting tensor equation can be rewritten in another form. Since then : where is the Schwarzschild radius, is the 4-speed, is the gravitational mass. This record reveals the physical meaning of . In a small area of space-time is almost flat and this equation can be written in the operator form : Then commutator operators and is : From here follow the specified uncertainty relations Substituting the values of and and cutting right and left of the same symbols, we obtain the Heisenberg uncertainty principle : In the particular case of a static spherically symmetric field and static distribution of matter and have remained : where is the Schwarzschild radius, is the radial coordinate. Last uncertainty relation allows make us some estimates of the equations of general relativity at the Planck scale. For example, the equation for the invariant interval в in the Schwarzschild solution has the form : Substitute according to the uncertainty relations . We obtain : It is seen that at the Planck scale space-time metric is bounded below by the Planck length, and on this scale, there are real and virtual Planckian black holes. Similar estimates can be made in other equations of general relativity. For example, analysis of the Hamilton-Jacobi equation for a centrally symmetric gravitational field in spaces of different dimensions indicates a preference for three-dimensional space for the emergence of virtual black holes . Prescribed above uncertainty relation valid for strong gravitational fields, as in any sufficiently small domain of a strong field space-time is essentially flat.".