The renormalized energy-momentum tensor and Casimir effect of Dirac field in two-dimensional static spacetime; 二维静态时空中Dirac场的重正化能动张量和Casimir效应 更多例句>> 5) ideal fluid 理想流体 1. Effect of sediment model on dynamic pressure in overlying ideal fluid due to P wave incidence...
A new class of exact solutions of Einstein's field equations with the energy-momentum tensor of a perfect fluid is given. The class of solutions is invariantly characterized by means of the following properties: (i) The energy-momentum tensor describes a perfect fluid. (ii) There are two ...
The perfect fluid energy-momentum tensor components relative to a coordinate basis read (15) where p () is the perfect fluid pressure (energy density) and are the components of the metric tensor. The elements of the perfect fluid follow circular trajectories, i.e., their four-velocity, read...
In particular, forD = 3and the LagrangeanLas any function of the above-mentioned invariant, the(r = 1)-field has energy-momentum tensor identical with that of a perfect fluid whose equation of state depends on the choice ofL(I).doi:10.1142/9789812834300_0140NIKOLAI V. MITSKIEVICH...
The diagonalization of the energy-momentum tensor of the disks is facilitated in this case by the fact that it can be written as an upper right triangular matrix. We find that the inclusion of electromagnetic fields changes significantly the different material properties of the disks and so we ...
Coupling the energy-momentum tensor for pressureless dust or fluid to the Einstein–Langevin equations, a modification of the Oppenheimer–Snyder dust collapse model is derived. The Einstein–Langevin field equations for the collapse are of the form of a Langevin equation for a non-linear Brownian ...
The equations of motion, the laws that govern the evolutions of the spin and color-charge tensors, and the expression for the energy-momentum tensor for the fluid in question are obtained. In the limiting case, the theory goes over to the well-known theory of Weyssenhoff-Raabe perfect ...
The energy-momentum tensor (EMT) for a perfect fluid, , takes the form T µν = (ρ +p) u µ u ν −pg µν , (2.4) where u µ ,ρ and p denote, respectively, the four-velocity, energy density and pressure of the fluid. Using gauge freedom (2.3) we choose the...
Summary The stress-energy tensor for the perfect magnetofluid is considered to show that i) the energy variation is affected by the magnetic field, and ii) the energy density and the matter density conserve along the flow vector if and only if the magnitude of the magnetic field conserves alo...
The Einstein’s Equations read Gµν = κTµν (1) and for any metric ˜gµν, an Einstein tensor ˜Gµν can be calculated; so, the metric ˜gµν can be claimed to solve Einstein’s Equations for the source given by the stress-energy-momentum tensor ˜T ...