Gravitational energy

For two pairwise interacting point particles, the gravitational potential energy U is the work that an outside agent must do in order to quasi-statically bring the masses together (which is therefore, exactly opposite the work done by the gravitational field on the masses): U = -W_g = -\int \vec{F}_g \cdot d\vec{r} where d\vec{r} is the displacement vector of the mass, \vec{F_g} is gravitational force acting on it and \cdot denotes scalar product. == Newtonian mechanics ==

In classical mechanics, two or more masses always have a gravitational potential. Conservation of energy requires that this gravitational field energy is always negative, so that it is zero when the objects are infinitely far apart. The gravitational potential energy is the potential energy an object has because it is within a gravitational field. The magnitude & direction of gravitational force experienced by a point mass m, due to the presence of another point mass M at a distance r, is given by Newton's law of gravitation. Taking origin to be at the position of M,\vec{F_g} = -\frac {GMm}{r^2}\hat{r}To get the total work done by the gravitational force in bringing point mass m from infinity to final distance R (for example, the radius of Earth) from point mass M, the force is integrated with respect to displacement: W_g = \int \vec{F}_g \cdot d\vec{r} = -\int_\infty^R \frac {GMm}{r^2}dr = \left . \frac{G M m}{r} \right|_{\infty}^{R} = \frac{G M m}{R}Gravitational potential energy being the minimum (quasi-static) work that needs to be done against gravitational force in this procedure,{{Equation box 1 |title=Gravitational Potential Energy |equation=U = -\frac {GMm}{R}}} Simplified version for Earth's surface In the common situation where a much smaller mass m is moving near the surface of a much larger object with mass M, the gravitational field is nearly constant and so the expression for gravitational energy can be considerably simplified. The change in potential energy moving from the surface (a distance R from the center) to a height h above the surface is \begin{align} \Delta U &= \frac{GMm}{R}-\frac{GMm}{R+h} \\ &= \frac{GMm}{R}\left(1-\frac{1}{1+h/R}\right) \end{align} If h/R is small, as it is close to the Earth's surface and where g can be considered constant over h, then this expression can be simplified using the binomial approximation \frac{1}{1+h/R} \approx 1-\frac{h}{R} to \begin{align} \Delta U &\approx \frac{GMm}{R}\left[1-\left(1-\frac{h}{R}\right)\right] \\ \Delta U &\approx \frac{GMmh}{R^2}\\ \Delta U &\approx m\left(\frac{GM}{R^2}\right)h \end{align} since the acceleration due to gravity is g = GM / R^2, this can be simplified to \Delta U \approx mgh Note, this is the change in potential energy in gaining some height h from the surface. == General relativity ==

("world lines"). According to general relativity, mass distorts spacetime and gravity is a natural consequence of Newton's First Law. Mass tells spacetime how to bend, and spacetime tells mass how to move. In general relativity gravitational energy is extremely complex, and there is no single agreed upon definition of the concept. It is sometimes modelled via the Landau–Lifshitz pseudotensor that allows retention for the energy–momentum conservation laws of classical mechanics. Addition of the matter stress–energy tensor to the Landau–Lifshitz pseudotensor results in a combined matter plus gravitational energy pseudotensor that has a vanishing 4-divergence in all frames—ensuring the conservation law. Some people object to this derivation on the grounds that pseudotensors are inappropriate in general relativity, but the divergence of the combined matter plus gravitational energy pseudotensor is a tensor. == See also ==