Kepler problem

Kepler problem

In classical mechanics, Kepler’s problem is a special case of the two-body problem, in which the two bodies interact by a central force F that varies in strength as the inverse square of the distance "r" between them. The force may be either attractive or repulsive. The "problem" to be solved is to find the position or speed of the two bodies over time given their masses and initial positions and velocities. Using classical mechanics, the solution can be expressed as a Kepler orbit using six orbital elements.

The Kepler problem is named after Johannes Kepler, who proposed Kepler's laws of planetary motion (which are part of classical mechanics and solve the problem for the orbits of the planets) and investigated the types of forces that would result in orbits obeying those laws (called "Kepler's inverse problem").cite book | last=Goldstein | first=H. | authorlink=Herbert Goldstein | year=1980 | title=Classical Mechanics | edition=2nd edition | publisher=Addison Wesley]


The Kepler problem arises in many contexts, some beyond the physics studied by Kepler himself. The Kepler problem is important in celestial mechanics, since Newtonian gravity obeys an inverse square law. Examples include a satellite moving about a planet, a planet about its sun, or two binary stars about each other. The Kepler problem is also important in the motion of two charged particles, since Coulomb’s law of electrostatics also obeys an inverse square law. Examples include the hydrogen atom, positronium and muonium, which have all played important roles as model systems for testing physical theories and measuring constants of nature.Facts|date=August 2008

The Kepler problem and the simple harmonic oscillator problem are the two most fundamental problems in classical mechanics. They are the "only" two problems that have closed orbits, i.e., return to their starting point with the same velocity (Bertrand's theorem). The Kepler problem has often been used to develop new methods in classical mechanics, such as Lagrangian mechanics, Hamiltonian mechanics, the Hamilton-Jacobi equation, and action-angle coordinates.Facts|date=August 2008 The Kepler problem also conserves the Laplace-Runge-Lenz vector, which has since been generalized to include other interactions. The solution of the Kepler problem allowed scientists to show that planetary motion could be explained entirely by classical mechanics and Newton’s law of gravity; the scientific explanation of planetary motion played an important role in ushering in the Enlightenment.

The Kepler problem in general relativity can be solved to produce more accurate predictions than by using classical mechanics, especially in the case of strong gravitational fields.

Mathematical definition

The central force F that varies in strength as the inverse square of the distance "r" between them:

:mathbf{F} = frac{k}{r^{2 mathbf{hat{r

where "k" is a constant and mathbf{hat{r represents the unit vector along the line between them. [cite book | last = Arnold | first = VI | authorlink = Vladimir Arnold | year = 1989 | title = Mathematical Methods of Classical Mechanics, 2nd ed. | publisher = Springer-Verlag | location = New York | pages = 38 | id = ISBN 0-387-96890-3] The force may be either attractive ("k"<0) or repulsive ("k">0). The corresponding scalar potential (the potential energy of the non-central body) is:

:V(r) = frac{k}{r}

olution of the Kepler problem

The equation of motion for the radius r of a particle of mass m moving in a central potential V(r) is given by Lagrange's equations

:mfrac{d^{2}r}{dt^{2 - mr omega^{2} = mfrac{d^{2}r}{dt^{2 - frac{L^{2{mr^{3 = -frac{dV}{dr}

where omega equiv frac{d heta}{dt} and the angular momentum L = mr^{2}omega is conserved. For illustration, the first term on the left-hand side is zero for circular orbits, and the applied inwards force frac{dV}{dr} equals the centripetal force requirement mr omega^{2}, as expected.

The definition of angular momentum allows a change of independent variable from t to heta

:frac{d}{dt} = frac{L}{mr^{2 frac{d}{d heta}

giving the new equation of motion that is independent of time

:frac{L}{r^{2 frac{d}{d heta} left( frac{L}{mr^{2 frac{dr}{d heta} ight)- frac{L^{2{mr^{3 = -frac{dV}{dr}

This equation becomes quasilinear on making the change of variables u equiv frac{1}{r} and multiplying both sides by frac{mr^{2{L^{2

:frac{d^{2}u}{d heta^{2 + u = -frac{m}{L^{2 frac{d}{du} V(1/u)

For an inverse-square force law such as the gravitational or electrostatic potential, the potential can be written

:V(mathbf{r}) = frac{k}{r} = ku The orbit u( heta) can be derived from the general equation

:frac{d^{2}u}{d heta^{2 + u = -frac{m}{L^{2 frac{d}{du} V(1/u) = -frac{km}{L^{2

whose solution is the constant -frac{km}{L^{2 plus a simple sinusoid

:u equiv frac{1}{r} = -frac{km}{L^{2 left [ 1 + e cos left( heta - heta_{0} ight) ight]

where e (the eccentricity) and heta_{0} (the phase offset) are constants of integration.

This is the general formula for a conic section that has one focus at the origin; e=0 corresponds to a circle, e<1 corresponds to an ellipse, e=1 corresponds to a parabola, and e>1 corresponds to a hyperbola. The eccentricity e is related to the total energy E (cf. the Laplace-Runge-Lenz vector)

:e = sqrt{1 + frac{2EL^{2{k^{2}m

Comparing these formulae shows that E<0 corresponds to an ellipse (all solutions which are closed orbits are ellipses), E=0 corresponds to a parabola, and E>0 corresponds to a hyperbola. In particular, E=-frac{k^{2}m}{2L^{2 for perfectly circular orbits (the central force exactly equals the centripetal force requirement, which determines the required angular velocity for a given circular radius).

For a repulsive force ("k">0) only e>1 applies.

ee also

* Kepler orbit
* Kepler's laws of planetary motion
* Kepler problem in general relativity
* Laplace-Runge-Lenz vector
* Bertrand's theorem
* Hamilton-Jacobi equation
* Action-angle coordinates


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