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In celestial mechanics, the gravitational potential belonging to an individual massive object, such as the earth or the sun, is a scalar field generated by that object, see also gravitational well. It is in every way analogous to the electric potential with mass playing the role of charge; the gravitational field is analogous to the electric field, and so are their mathematics and properties.

In mathematics the gravitational potential is also known as the Newtonian potential and is fundamental in the study of potential theory.

Mathematical form

The potential V at point b located a distance r from a point mass at point a is given by:

${\displaystyle V=-{\frac {GM}{r}},}$

where M is the mass at point a and G is the gravitational constant (6.67428 × 10 N (m/kg)).

The potential, V, has dimensions of energy per unit mass, and it approaches an upper limit of zero as r approaches infinity.

More generally, the potential associated with any mass distribution is obtained by the superposition of potential associated with the individual masses. In the case of discrete point masses, this is the algebraic sum of the gravitational potentials. The potentialat point b is given by

${\displaystyle V(\mathbf {r} )=-\sum _{i}{\frac {GM_{i}}{|\mathbf {R} -\mathbf {r} _{i}|}}\,{\rm {where\ \mathbf {r} =|\mathbf {R} -\mathbf {r} _{i}|\ }}}$ and where R is a vector from the center of mass to point b.

For the continuous case the potential, V at point b, is computed as an integral over the distributed mass,

${\displaystyle V(\mathbf {r} )=-\int {\frac {G}{|\mathbf {R} -\mathbf {x} |}}\ dm}$ where dm equals density times differential volume and where x is a vector from the center of mass to the differential element of mass.

Expanding the denominator by taking the square root of the square, carrying out the dot product, and factoring R out of the denominator we get the more useful expression,

${\displaystyle V(\mathbf {r} )=-\int {\frac {G}{\sqrt {R^{2}-2\mathbf {R} \cdot \mathbf {x} +x^{2}}}}\,dm=-{\frac {1}{R}}\int G\,/\,{\sqrt {1-2cos(\beta ){\frac {x}{R}}+\left({\frac {x}{R}}\right)^{2}}}\,dm.}$

The gravitational field, and thus the acceleration of a (small) body in the space around the massive object, is given by the negative gradient of the gravitational potential. The gravitational field associated to a point mass follows an inverse square law: the magnitude of the observed acceleration is

${\displaystyle \left|\mathbf {a} \right|={\frac {GM}{r^{2}}}.}$

The direction of the acceleration is towards the point mass. Thus the acceleration vector is

${\displaystyle \mathbf {a} =-{\frac {GM}{r^{3}}}\mathbf {r} =-{\frac {GM}{r^{2}}}{\hat {\mathbf {r} }}.}$

Spherical symmetry

A spherically symmetric mass distribution behaves to an observer completely outside the distribution as though all of the mass were concentrated at the center, and thus effectively as a point mass, by the shell theorem. On the surface of the Earth, the acceleration is given by so-called standard gravity g, approximately 9.8 m/s, although this value varies slightly with latitude and altitude: the magnitude of the acceleration is a little larger at the poles than at the equator because the Earth is an oblate spheroid.

Within a spherically symmetric mass distribution, it is possible to solve Poisson's equation in spherical coordinates. Within a uniform spherical body of radius R and density σ, the gravitational force g inside the sphere varies linearly with distance r from the center, giving the gravitational potential inside the sphere, which is

${\displaystyle V(r)={\frac {2}{3}}\pi G\sigma (r^{2}-3R^{2}),\qquad r\leq R,}$

which smoothly connects to the potential function for the outside of the sphere (see the figure at the top).

Potential energy

The gravitational potential (V) is the potential energy (U) per unit mass:

${\displaystyle U=mV}$

where m is the mass of the object. The potential energy is the negative of the work done by the gravitational field moving the body to its given position in space from infinity. If the body has a mass of 1 unit, then the potential energy to be assigned to that body is equal to the gravitational potential. So the potential can be interpreted as the negative of the work done by the gravitational field moving a unit mass in from infinity.

In some situations the equations can be simplified by assuming a field which is nearly independent of position. For instance, in daily life, in the region close to the surface of the Earth, the gravitational acceleration can be considered constant. In that case the difference in potential energy from one height to another is to a good approximation linearly related to the difference in height:

${\displaystyle \Delta U=mg\Delta h}$

General relativity

In general relativity, the gravitational potential is replaced by the metric tensor.

References

• Peter Dunsby (1996-06-15). "Mass in Newtonian theory". Tensors and Relativity: Chapter 5 Conceptual Basis of General Relativity. Department of Mathematics and Applied Mathematics University of Cape Town. Retrieved 2009-03-25.
• Lupei Zhu Associate Professor, Ph.D. (California Institute of Technology, 1998). "Gravity and Earth's Density Structure". EAS-437 Earth Dynamics. Saint Louis University (Department of Earth and Atmospheric Sciences). Retrieved 2009-03-25.{{cite web}}: CS1 maint: multiple names: authors list (link) CS1 maint: numeric names: authors list (link)
• Charles D. Ghilani (2006-11-28). "The Gravity Field of the Earth". The Physics Fact Book. Penn State Surveying Engineering Program. Retrieved 2009-03-25.
• Rastall, Peter (1991). Postprincipia: Gravitation for Physicists and Astronomers. World Scientific. pp. 7ff. ISBN 9810207786.
• Vladimirov, V. S. (1971), Equations of mathematical physics, Translated from the Russian by Audrey Littlewood. Edited by Alan Jeffrey. Pure and Applied Mathematics, vol. 3, New York: Marcel Dekker Inc., MR0268497.

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