Tidal tensor

In Newton's theory of gravitation and in various relativistic classical theories of gravitation, such as general relativity, the tidal tensor represents

1. tidal accelerations of a cloud of (electrically neutral, nonspinnig) test particles,
2. tidal stresses in a small object immersed in an ambient gravitational field.

Newton's theory

In the field theoretic elaboration of Newtonian gravity, the central quantity is the gravitational potential $\phi$, which obeys the Poisson equation

$\Delta \phi =4\pi \,\mu$

where $\mu$ is the maass density of any matter present. Note that this equation implies that in a vacuum solution, the potential is simply a harmonic function.

The tidal tensor is given by the traceless part $J_{ab}-{\frac {1}{3}}\,{J^{m}}_{m}\,\eta _{ab}$ of the Hessian

$J_{ab}={\frac {\partial ^{2}\phi }{\partial x^{a}\,\partial x^{b}}}$

where we are using the standard Cartesian chart for E³, with the euclidean metric tensor

$ds^{2}=dx^{2}+dy^{2}+dz^{2}$

Using standard results in vector calculus, this is readily converted to expressions valid in other coordinate charts, such as the polar spherical chart

$ds^{2}=d\rho ^{2}+\rho ^{2}\,\left(d\theta ^{2}+\sin(\theta )^{2}\,d\phi ^{2}\right)$

Spherically symmetric field

As an example, we compute the tidal tensor for the vacuum field outside an isolated spherically symmetric massive object.

First, let us compare the gravitational forces on two nearby observers lying on the same radial line:

$m/(r+h)^{2}-m/r^{2}=-2m/r^{3}\,h+3m/r^{4}\,h^{2}+O(h^{3})$

Because in discussing tensors we are dealing with multilinear algebra, we retain only first order terms, so $\Phi _{11}=-2m/r^{3}$. Similarly, we can compare the gravitational force on two nearby observers lying on the same sphere $r=r_{0}$. Using some elementary trigonometry and the small angle approximation, we find that the force vectors differ by a vector tangent to the sphere which has magnitude

${\frac {m}{r_{0}^{2}}}\,\sin(\theta )\approx {\frac {m}{r_{0}^{2}}}\,{\frac {h}{r_{0}}}={\frac {m}{r_{0}^{3}}}\,h$

By using the small angle approximation, we have ignored all terms of order $O(h^{2})$, so the tangential components are $\Phi _{22}=\Phi _{33}=m/r^{3}$. Here, we are referring to the obvious frame obtained from the polar spherical chart for our three-dimensional euclidean space:

${\vec {\epsilon }}_{1}=\partial _{r},\;{\vec {\epsilon }}_{2}={\frac {1}{r}}\,\partial _{\theta },\;{\vec {\epsilon }}_{3}={\frac {1}{r\sin \theta }}\,\partial _{\phi }$

General relativity

In general relativity, the tidal tensor is identified with the electrogravitic tensor, which is one piece of the Bel decomposition of the Riemann tensor.