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Astrodynamics 

In classical mechanics, the twobody problem is to predict the motion of two massive objects which are abstractly viewed as point particles. The problem assumes that the two objects interact only with one another; the only force affecting each object arises from the other one, and all other objects are ignored.
The most prominent case of the classical twobody problem is the gravitational case (see also Kepler problem), arising in astronomy for predicting the orbits (or escapes from orbit) of objects such as satellites, planets, and stars. A twopointparticle model of such a system nearly always describes its behavior well enough to provide useful insights and predictions.
A simpler "one body" model, the "centralforce problem", treats one object as the immobile source of a force acting on the other. One then seeks to predict the motion of the single remaining mobile object. Such an approximation can give useful results when one object is much more massive than the other (as with a light planet orbiting a heavy star, where the star can be treated as essentially stationary).
However, the onebody approximation is usually unnecessary except as a stepping stone. For many forces, including gravitational ones, the general version of the twobody problem can be reduced to a pair of onebody problems, allowing it to be solved completely, and giving a solution simple enough to be used effectively.
By contrast, the threebody problem (and, more generally, the nbody problem for n ≥ 3) cannot be solved in terms of first integrals, except in special cases.
The twobody problem is interesting in astronomy because pairs of astronomical objects are often moving rapidly in arbitrary directions (so their motions become interesting), widely separated from one another (so they will not collide) and even more widely separated from other objects (so outside influences will be small enough to be ignored safely).
Under the force of gravity, each member of a pair of such objects will orbit their mutual center of mass in an elliptical pattern, unless they are moving fast enough to escape one another entirely, in which case their paths will diverge along other planar conic sections. If one object is very much heavier than the other, it will move far less than the other with reference to the shared center of mass. The mutual center of mass may even be inside the larger object.
For the derivation of the solutions to the problem, see Classical centralforce problem or Kepler problem.
In principle, the same solutions apply to macroscopic problems involving objects interacting not only through gravity, but through any other attractive scalar force field obeying an inversesquare law, with electrostatic attraction being the obvious physical example. In practice, such problems rarely arise. Except perhaps in experimental apparatus or other specialized equipment, we rarely encounter electrostatically interacting objects which are moving fast enough, and in such a direction, as to avoid colliding, and/or which are isolated enough from their surroundings.
The dynamical system of a twobody system under the influence of torque turns out to be a SturmLiouville equation.^{[1]}
Although the twobody model treats the objects as point particles, classical mechanics only apply to systems of macroscopic scale. Most behavior of subatomic particles cannot be predicted under the classical assumptions underlying this article or using the mathematics here.
Electrons in an atom are sometimes described as "orbiting" its nucleus, following an early conjecture of Niels Bohr (this is the source of the term "orbital"). However, electrons don't actually orbit nuclei in any meaningful sense, and quantum mechanics are necessary for any useful understanding of the electron's real behavior. Solving the classical twobody problem for an electron orbiting an atomic nucleus is misleading and does not produce many useful insights.
This section duplicates the scope of other articles, specifically Classical centralforce problem#Relation to the classical twobody problem. (June 2019) 
The complete twobody problem can be solved by reformulating it as two onebody problems: a trivial one and one that involves solving for the motion of one particle in an external potential. Since many onebody problems can be solved exactly, the corresponding twobody problem can also be solved.
Let x_{1} and x_{2} be the vector positions of the two bodies, and m_{1} and m_{2} be their masses. The goal is to determine the trajectories x_{1}(t) and x_{2}(t) for all times t, given the initial positions x_{1}(t = 0) and x_{2}(t = 0) and the initial velocities v_{1}(t = 0) and v_{2}(t = 0).
When applied to the two masses, Newton's second law states that

(Equation 1) 

(Equation 2) 
where F_{12} is the force on mass 1 due to its interactions with mass 2, and F_{21} is the force on mass 2 due to its interactions with mass 1. The two dots on top of the x position vectors denote their second derivative with respect to time, or their acceleration vectors.
Adding and subtracting these two equations decouples them into two onebody problems, which can be solved independently. Adding equations (1) and (2) results in an equation describing the center of mass (barycenter) motion. By contrast, subtracting equation (2) from equation (1) results in an equation that describes how the vector r = x_{1} − x_{2} between the masses changes with time. The solutions of these independent onebody problems can be combined to obtain the solutions for the trajectories x_{1}(t) and x_{2}(t).
Let be the position of the center of mass (barycenter) of the system. Addition of the force equations (1) and (2) yields
The resulting equation:
Dividing both force equations by the respective masses, subtracting the second equation from the first, and rearranging gives the equation
The force between the two objects, which originates in the two objects, should only be a function of their separation r and not of their absolute positions x_{1} and x_{2}; otherwise, there would not be translational symmetry, and the laws of physics would have to change from place to place. The subtracted equation can therefore be written:
Solving the equation for r(t) is the key to the twobody problem. The solution depends on the specific force between the bodies, which is defined by . For the case where follows an inversesquare law, see the Kepler problem.
Once R(t) and r(t) have been determined, the original trajectories may be obtained
The motion of two bodies with respect to each other always lies in a plane (in the center of mass frame).
Proof: Defining the linear momentum p and the angular momentum L of the system, with respect to the center of mass, by the equations
where μ is the reduced mass and r is the relative position r_{2} − r_{1} (with these written taking the center of mass as the origin, and thus both parallel to r) the rate of change of the angular momentum L equals the net torque N
Introducing the assumption (true of most physical forces, as they obey Newton's strong third law of motion) that the force between two particles acts along the line between their positions, it follows that r × F = 0 and the angular momentum vector L is constant (conserved). Therefore, the displacement vector r and its velocity v are always in the plane perpendicular to the constant vector L.
If the force F(r) is conservative then the system has a potential energy U(r), so the total energy can be written as
In the center of mass frame the kinetic energy is the lowest and the total energy becomes
For many physical problems, the force F(r) is a central force, i.e., it is of the form