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fluid solution : ウィキペディア英語版
fluid solution
In general relativity, a fluid solution is an exact solution of the Einstein field equation in which the gravitational field is produced entirely by the mass, momentum, and stress density of a fluid.
In astrophysics, fluid solutions are often employed as stellar models. (It might help to think of a perfect gas as a special case of a perfect fluid.) In cosmology, fluid solutions are often used as cosmological models.
==Mathematical definition==

The stress–energy tensor of a relativistic fluid can be written in the form
:T^ = \mu \, u^a \, u^b + p \, h^ + \left( u^a \, q^b + q^a \, u^b \right) + \pi^
Here
* the world lines of the fluid elements are the integral curves of the velocity vector u^a,
* the projection tensor h_ = g_ + u_a \, u_b projects other tensors onto hyperplane elements orthogonal to u^a,
* the matter density is given by the scalar function \mu,
* the pressure is given by the scalar function p,
* the heat flux vector is given by q^a,
* the viscous shear tensor is given by \pi^.
The heat flux vector and viscous shear tensor are ''transverse'' to the world lines, in the sense that
:q_a \, u^a = 0, \; \; \pi_ \, u^b = 0
This means that they are effectively three-dimensional quantities, and since the viscous stress tensor is symmetric and traceless, they have respectively 3 and 5 linearly independent components. Together with the density and pressure, this makes a total of 10 linearly independent components, which is the number of linearly independent components in a four-dimensional symmetric rank two tensor.

抄文引用元・出典: フリー百科事典『 ウィキペディア(Wikipedia)
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