List of Figures

View Image Figure 1:
A “timeline” focussed on the topics covered in this review, including chemists, engineers, mathematicians, philosophers, and physicists who have contributed to the development of non-relativistic fluids, their relativistic counterparts, multi-fluid versions of both, and exotic phenomena such as superfluidity.
View Image Figure 2:
A schematic illustration of two possible versions of parallel transport. In the first case (a) a vector is transported along great circles on the sphere locally maintaining the same angle with the path. If the contour is closed, the final orientation of the vector will differ from the original one. In case (b) the sphere is considered to be embedded in a three-dimensional Euclidean space, and the vector on the sphere results from projection. In this case, the vector returns to the original orientation for a closed contour.
View Image Figure 3:
A schematic illustration of the Lie derivative. The coordinate system is dragged along with the flow, and one can imagine an observer “taking derivatives” as he/she moves with the flow (see the discussion in the text).
View Image Figure 4:
The projections at point P of a vector μ V onto the worldline defined by μ U and into the perpendicular hypersurface (obtained from the action of ⊥ μν).
View Image Figure 5:
An object with a characteristic size D is modeled as a fluid that contains M fluid elements. From inside the object we magnify a generic fluid element of characteristic size L. In order for the fluid model to work we require M ≫ N ≫ 1 and D ≫ L.
View Image Figure 6:
A local, geometrical view of the Euler equation as an integrability condition of the vorticity for a single-constituent perfect fluid.
View Image Figure 7:
The push-forward from “fluid-particle” points in the three-dimensional matter space labelled by the coordinates {X1, X2, X3 } to fluid-element worldlines in spacetime. Here, the push-forward of the “Ith” (I = 1,2,...,n) fluid-particle to, say, an initial point on a worldline in spacetime can be taken as A A i X I = X (0, xI) where i xI is the spatial position of the intersection of the worldline with the t = 0 time slice.
View Image Figure 8:
The push-forward from a point in the th x-constituent’s three-dimensional matter space (on the left) to the corresponding “fluid-particle” worldline in spacetime (on the right). The points in matter space are labelled by the coordinates {X1x,X2x,X3x}, and the constituent index x = n,s. There exist as many matter spaces as there are dynamically independent fluids, which for this case means two.