Observational constraintsPhysical parametersIn this study, we explore cosmological models within the framework off(T)gravity by utilizing the energy–momentum tensor for a perfect fluid to solve the corresponding field equations. We derive key cosmological parameters, including the Hubble parameterH. ...
The perfect fluid energy-momentum tensor components Tμν relative to a coordinate basis read Tμν = ( p + ρ)UμUν − pgμν (15) where p (ρ) is the perfect fluid pressure (energy density) and gμν are the components of the metric tensor. The ele- ments of the perfect ...
The perfect fluid energy-momentum tensor components Tμν relative to a coordinate basis read Tμν=(p+ρ)UμUν−pgμν (15) where p (ρ) is the perfect fluid pressure (energy density) and gμν are the components of the metric tensor. The elements of the perfect fluid follow ci...
The application of the whole structure of a Lagrangian theory with an appropriate choice of Lagrangian invariant as the pressure of the fluid shows that the Euler-Lagrange equations with their corresponding energy-momentum tensors lead to Navier-Stokes' equation identical with the Euler equation for ...
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...
energy-momentum tensor diagonalizationThe interpretation of a family of electrovacuum stationary Taub-NUT-type fields in terms of finite charged perfect fluid disks is presented. The interpretation is made by means of an "inverse problem" approach used to obtain disk sources of known solutions of ...
Here α(ϕ) = d ln(A(ϕ))/dϕ, and the Einstein frame energy-momentum tensor T µν is related to the Jordan frame one ˜ T µν via T µν = A 2 (ϕ) ˜ T µν . In the case of a perfect fluid one has ρ = A 4 (ϕ)˜ ρ, p = A 4 (ϕ...
The energy-momentum tensor of the charged scalar field is expressed as follows:(29)⁎⁎⁎⁎⁎⁎Tνμ=12DμΨ∂νΨ⁎+12D⁎μΨ⁎∂νΨ−δνμ[12DαΨD⁎αΨ⁎−12μsΨΨ⁎], with(30)D=∂μ−iqAμ. The energy flux through the event horizon can be ...
We are interested in the perfect fluid solutions, the stress-energy-momentum tensor can be written as Tμν=(ρ(r)+p(r))uμuν+p(r)gμν, whereuμis the proper velocity. We also assume that both the the energy densityρ(r)and the fluid pressurep(r)depend only on the radial coo...
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...