Classical central-force problem

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In classical mechanics, the central-force problem is to determine the motion of a particle under the influence of a single central force. A central force is a force that points from the particle directly towards (or directly away from) a fixed point in space, the center, and whose magnitude only depends on the distance of the object to the center. In many important cases, the problem can be solved analytically, i.e., in terms of well-studied functions such as trigonometric functions.

The solution of this problem is important to classical physics, since many naturally occurring forces are central. Examples include gravity and electromagnetism as described by Newton's law of universal gravitation and Coulomb's law, respectively. The problem is also important because some more complicated problems in classical physics (such as the two-body problem with forces along the line connecting the two bodies) can be reduced to a central-force problem. Finally, the solution to the central-force problem often makes a good initial approximation of the true motion, as in calculating the motion of the planets in the Solar System.

Basics[edit]

The essence of the central-force problem is to solve for the position r[note 1] of a particle moving under the influence of a central force F, either as a function of time t or as a function of the angle φ relative to the center of force and an arbitrary axis.

Definition of a central force[edit]

A long arrows runs from the lower left to the upper right. At the lower left, the arrow begins with a black point labeled "O"; at the upper right, the arrow ends at a solid red circle labeled "P". Above this arrow is a shorter, thicker arrow labeled "F sub att" that points from the center of P towards O.
An attractive central force acting on a body at position P (shown in red). By definition, a central force must point either towards a fixed point O (if attractive) or away from it (if repulsive).

A central force F has two defining properties.[1] First, it must drive particles either directly towards or directly away from a fixed point in space, the center of force, which is often labeled O. In other words, a central force must act along the line joining O with the present position of the particle. Second, a central force depends only on the distance r between O and the moving particle; it does not depend explicitly on time or other descriptors of position.

This two-fold definition may be expressed mathematically as follows. The center of force O can be chosen as the origin of a coordinate system. The vector r joining O to the present position of the particle is known as the position vector. Therefore, a central force must have the mathematical form[2]


\mathbf{F} = F(r)\hat{\mathbf{r}}

where r is the vector magnitude |r| (the distance to the center of force) and = r/r is the corresponding unit vector. According to Newton's second law of motion, the central force F generates a parallel acceleration a scaled by the mass m of the particle[note 2]


\mathbf{F} = F(r) \hat{\mathbf{r}} = m\mathbf{a} = m \ddot{\mathbf{r}}

For attractive forces, F(r) is negative, because it works to reduce the distance r to the center. Conversely, for repulsive forces, F(r) is positive.

Potential energy[edit]

A central force is always a conservative force; the magnitude F(r) of a central force can always be expressed as the derivative of a time-independent potential energy function U(r)[3]


F(r) = -\frac{dU}{dr}

Thus, the total energy of the particle—the sum of its kinetic energy and its potential energy U—is a constant; energy is said to be conserved. To show this, it suffices that the work W done by the force depends only on initial and final positions, not on the path taken between them.


W = \int_{\mathbf{r}_{1}}^{\mathbf{r}_{2}} \mathbf{F} \cdot d\mathbf{r} = \int_{\mathbf{r}_{1}}^{\mathbf{r}_{2}} F(r) \hat{\mathbf{r}} \cdot d\mathbf{r} = \int_{r_{1}}^{r_{2}} F dr = U(r_{1}) - U(r_{2})

Equivalently, it suffices that the curl of the force field F is zero; using the formula for the curl in spherical coordinates,


\nabla \times \mathbf{F} = \frac{1}{r \sin \theta} \left( \frac{\partial F}{\partial \varphi} \right) \hat{\boldsymbol\theta} - \frac{1}{r} \left( \frac{\partial F}{\partial \theta} \right) \hat{\boldsymbol\varphi} = 0

because the partial derivatives are zero for a central force; the magnitude F does not depend on the angular spherical coordinates θ and φ.

Since the scalar potential V(r) depends only on the distance r to the origin, it has spherical symmetry. In this respect, the central-force problem is analogous to the Schwarzschild geodesics in general relativity and to the quantum mechanical treatments of particles in potentials of spherical symmetry.

One-dimensional problem[edit]

If the initial velocity v of the particle is aligned with position vector r, then the motion remains forever on the line defined by r. This follows because the force—and by Newton's second law, also the acceleration a—is also aligned with r. To determine this motion, it suffices to solve the equation


m \ddot{r} = F(r)

One solution method is to use the conservation of total energy


|\dot{r}| = \Big| \frac{dr}{dt}\Big| = \sqrt{\frac{2}{m}} \sqrt{E_{\mathrm{tot}} - U(r)}

Taking the reciprocal and integrating we get:


|t - t_{0}| = {\sqrt{\frac{m}{2}}} \int \frac{|dr|}{\sqrt{E_{\mathrm{tot}} - U(r)}}

For the remainder of the article, it is assumed that the initial velocity v of the particle is not aligned with position vector r, i.e., that the angular momentum vector L = r × m v is not zero.

Uniform circular motion[edit]

Every central force can produce uniform circular motion, provided that the initial radius r and speed v satisfy the equation for the centripetal force


\frac{mv^{2}}{r} = F(r)

If this equation is satisfied at the initial moments, it will be satisfied at all later times; the particle will continue to move in a circle of radius r at speed v forever.

Relation to the classical two-body problem[edit]

The positions x1 and x2 of two bodies can be expressed in terms of their relative separation r and the position of their center of mass Rcm.

The central-force problem concerns an ideal situation (a "one-body problem") in which a single particle is attracted or repelled from an immovable point O, the center of force.[4] However, physical forces are generally between two bodies; and by Newton's third law, if the first body applies a force on the second, the second body applies an equal and opposite force on the first. Therefore, both bodies are accelerated if a force is present between them; there is no perfectly immovable center of force. However, if one body is overwhelmingly more massive than the other, its acceleration relative to the other may be neglected; the center of the more massive body may be treated as approximately fixed.[5] For example, the Sun is overwhelmingly more massive than the planet Mercury; hence, the Sun may be approximated as an immovable center of force, reducing the problem to the motion of Mercury in response to the force applied by the Sun. In reality, however, the Sun also moves (albeit only slightly) in response to the force applied by the planet Mercury.

Any classical two-body problem to be converted into an equivalent one-body problem. The mass μ of the one equivalent body equals the reduced mass of the two original bodies, and its position r equals the difference of their positions.

Such approximations are unnecessary, however. Newton's laws of motion allow any classical two-body problem to be converted into a corresponding exact one-body problem.[6] To demonstrate this, let x1 and x2 be the positions of the two particles, and let r = x1x2 be their relative position. Then, by Newton's second law,


\ddot{\mathbf{r}} = \ddot{\mathbf{x}}_{1} - \ddot{\mathbf{x}}_{2} = 
\left( \frac{\mathbf{F}_{21}}{m_{1}} - \frac{\mathbf{F}_{12}}{m_{2}} \right) =
\left(\frac{1}{m_{1}} + \frac{1}{m_{2}} \right)\mathbf{F}_{21}

The final equation derives from Newton's third law; the force of the second body on the first body (F21) is equal and opposite to the force of the first body on the second (F12). Thus, the equation of motion for r can be written in the form


\mu \ddot{\mathbf{r}} = \mathbf{F}

where \mu is the reduced mass


\mu = \frac{1}{\frac{1}{m_{1}} + \frac{1}{m_{2}}} = \frac{m_{1}m_{2}}{m_{1} + m_{2}}

As a special case, the problem of two bodies interacting by a central force can be reduced to a central-force problem of one body.

Qualitative properties[edit]

Planar motion[edit]

The image shows a yellow disc with three vectors. The vector L is perpendicular to the disk, the vector r goes from the center of the disk to a point on its periphery, and the vector v is tangential to the disk, starting from the point where r meets the periphery.
Illustration of planar motion. The angular momentum vector L is constant; therefore, the position vector r and velocity vector v must lie in the yellow plane perpendicular to L.

The motion of a particle under a central force F always remains in the plane defined by its initial position and velocity.[7] This may be seen by symmetry. Since the position r, velocity v and force F all lie in the same plane, there is never an acceleration perpendicular to that plane, because that would break the symmetry between "above" the plane and "below" the plane.

To demonstrate this mathematically, it suffices to show that the angular momentum of the particle is constant. This angular momentum L is defined by the equation


\mathbf{L} = \mathbf{r} \times \mathbf{p} = \mathbf{r} \times m \mathbf{v}

where m is the mass of the particle and p is its linear momentum.[note 3] Therefore, the angular momentum vector L is always perpendicular to the plane defined by the particle's position vector r and velocity vector v.[note 4]

In general, the rate of change of the angular momentum L equals the net torque r × F[8]


\frac{d\mathbf{L}}{dt} = \dot{\mathbf{r}} \times m\mathbf{v} + \mathbf{r} \times m\dot{\mathbf{v}} = \mathbf{v} \times m\mathbf{v} + \mathbf{r} \times \mathbf{F} = \mathbf{r} \times \mathbf{F} \ ,

The first term m v × v is always zero, because the vector cross product is always zero for any two vectors pointing in the same or opposite directions. However, when F is a central force, the remaining term r × F is also zero because the vectors r and F point in the same or opposite directions. Therefore, the angular momentum vector L is constant. Consequently, the particle's position r and velocity v always lie in a single plane perpendicular to L.[9]

Polar coordinates[edit]

Two perpendicular lines (Cartesian coordinate axes) are labeled x (horizontal) and y (vertical). They intersect at the lower left in a point labeled O (the origin). An arrow labeled r runs form the origin to the upper right, ending in a point P. The angle between the x-axis and the vector r is labeled with the Greek letter φ. A vertical line is dropped from P to the x-axis, and the horizontal and vertical segments are labeled "r cosine phi" and "r sine phi", respectively.
The position vector r of a point P in the plane can be specified by its distance r from the center (the origin O) and its azimuthal angle φ. The x and y Cartesian components of the vector are r cos φ and r sin φ, respectively.

Since the motion is planar and the force radial, it is customary to switch to polar coordinates.[9] In these coordinates, the position vector r is represented in terms of the radial distance r and the azimuthal angle φ.


\mathbf{r} = (x, \ y ) = r (\cos \varphi ,\ \sin \varphi)

Taking the first derivative with respect to time yields the particle's velocity vector v


\mathbf{v} = \frac{d\mathbf{r}}{dt} = \dot{r} (\cos \varphi ,\ \sin \varphi) + r \dot{\varphi} (-\sin \varphi, \cos \varphi)

Similarly, the second derivative of the particle's position r equals its acceleration a


\mathbf{a} =
\ddot{r} (\cos \varphi ,\ \sin \varphi) + 2 \dot{r} \dot{\varphi} (-\sin \varphi ,\ \cos \varphi) + 
r \ddot{\varphi} (-\sin \varphi, \cos \varphi)  - r \dot{\varphi}^{2}  (\cos \varphi, \sin \varphi)

The velocity v and acceleration a can be expressed in terms of the radial and azimuthal unit vectors. The radial unit vector is obtained by dividing the position vector r by its magnitude r, as described above


\mathbf{\hat{r}} = (\cos \varphi ,\ \sin \varphi)

The azimuthal unit vector is given by[note 5]


\hat{\boldsymbol\varphi} = (-\sin \varphi ,\ \cos \varphi)

Thus, the velocity can be written as


\mathbf{v} = v_{r}  \mathbf{\hat{r}} + v_{\varphi} \hat{\boldsymbol\varphi} = \dot{r} \mathbf{\hat{r}} + r\dot{\varphi} \hat{\boldsymbol\varphi}

whereas the acceleration equals


\mathbf{a} = a_{r}  \mathbf{\hat{r}} + a_{\varphi} \hat{\boldsymbol\varphi} = (\ddot{r} - r \dot{\varphi}^{2}) \mathbf{\hat{r}} + (2 \dot{r} \dot{\varphi} + r \ddot{\varphi} ) \hat{\boldsymbol\varphi}

Specific angular momentum[edit]

The specific angular momentum h equals the speed v times r, the component of the position vector r perpendicular to the velocity vector v. h also equals the radial distance r times the azimuthal component vφ of the velocity. Both of these formulae are equal to rv cos β.

Since F = ma by Newton's second law of motion and since F is a central force, then only the radial component of the acceleration a can be non-zero; the angular component aφ must be zero


a_{\varphi} = 2 \dot{r} \dot{\varphi} + r \ddot{\varphi}  = 0

Therefore


\frac{d}{dt} \left( r^{2} \dot{\varphi} \right) = r (2 \dot{r} \dot{\varphi} + r \ddot{\varphi}) = r a_{\varphi} = 0

This expression in parentheses is usually denoted h


h = r^{2} \dot{\varphi} = r v_{\varphi} = \left| \mathbf{r} \times \mathbf{v} \right| = v r_{\perp} = \frac{L}{m}

which equals the speed v times r, the component of the radius vector perpendicular to the velocity. h is the magnitude of the specific angular momentum because it equals the magnitude L of the angular momentum divided by the mass m of the particle.

For brevity, the angular speed is sometimes written ω


\omega = \dot{\varphi} = \frac{d\varphi}{dt}

However, it should not be assumed that ω is constant. Since h is constant, ω varies with the radius r according to the formula[10]


\omega = \frac{h}{r^{2}}

Since h is constant and r2 is positive, the angle φ changes monotonically in any central-force problem, either continuously increasing (h positive) or continuously decreasing (h negative).[11]

Constant areal velocity[edit]

Since the area A equals ½ rvt, the areal velocity dA/dt (the rate at which A is swept out by the particle) equals ½ rv = ½h.
See also: Areal velocity

The magnitude of h also equals twice the areal velocity, which is the rate at which area is being swept out by the particle relative to the center.[12] Thus, the areal velocity is constant for a particle acted upon by any type of central force; this is Kepler's second law.[13] Conversely, if the motion under a conservative force F is planar and has constant areal velocity for all initial conditions of the radius r and velocity v, then the azimuthal acceleration aφ is always zero. Hence, by Newton's second law, F = ma, the force is a central force.

The constancy of areal velocity may be illustrated by uniform circular and linear motion. In uniform circular motion, the particle moves with constant speed v around the circumference of a circle of radius r. Since the angular velocity ω = v/r is constant, the area swept out in a time Δt equals ω r2Δt; hence, equal areas are swept out in equal times Δt. In uniform linear motion (i.e., motion in the absence of a force, by Newton's first law of motion), the particle moves with constant velocity, that is, with constant speed v along a line. In a time Δt, the particle sweeps out an area ½vΔtr (the impact parameter).[note 6] The distance r does not change as the particle moves along the line; it represents the distance of closest approach of the line to the center O (the impact parameter). Since the speed v is likewise unchanging, the areal velocity ½vr is a constant of motion; the particle sweeps out equal areas in equal times.

The area A of a circular sector equals ½ r2φ = ½ r2ωt = ½ r vφt. Hence, the areal velocity dA/dt equals ½ r vφ = ½ h. For uniform circular motion, r and vφ are constant; thus, dA/dt is also constant.

Equivalent parallel force field[edit]

By a transformation of variables,[14] any central-force problem can be converted into an equivalent parallel-force problem.[note 7] In place of the ordinary x and y Cartesian coordinates, two new position variables ξ = x/y and η = 1/y are defined, as is a new time coordinate τ


\tau = \int \frac{dt}{y^{2}}

The corresponding equations of motion for ξ and η are given by


\frac{d\xi}{d\tau} = \frac{d}{dt} \left( \frac{x}{y} \right) \frac{dt}{d\tau} = \left( \frac{\dot{x} y - \dot{y} x}{y^{2}} \right) y^{2} = - h

\frac{d\eta}{d\tau} = \frac{d}{dt} \left( \frac{1}{y} \right) \frac{dt}{d\tau} = - \frac{\dot{y}}{y^{2}} y^{2} = -\dot{y}

Since the rate of change of ξ is constant, its second derivative is zero


\frac{d^{2}\xi}{d\tau^{2}} = 0

Since this is the acceleration in the ξ direction and since F=ma by Newton's second law, it follows that the force in the ξ direction is zero. Hence the force is only along the η direction, which is the criterion for a parallel-force problem. Explicitly, the acceleration in the η direction equals


\frac{d^{2}\eta}{d\tau^{2}} = \frac{dt}{d\tau} \frac{d}{dt} \left( \frac{d\eta}{d\tau} \right) = - y^{2} \ddot{y} = -\frac{y^{3}}{mr} F(r)

because the acceleration in the y-direction equals


\ddot{y} = \frac{1}{m} F_{y} = \frac{1}{m} F(r) \, \frac{y}{r}

Here, Fy denotes the y-component of the central force, and y/r equals the cosine of the angle between the y-axis and the radial vector r.

General solution[edit]

Binet equation[edit]

See also: Binet equation

Since a central force F acts only along the radius, only the radial component of the acceleration is nonzero. By Newton's second law of motion, the magnitude of F equals the mass m of the particle times the magnitude of its radial acceleration[15]


F(r) = 
m \ddot{r} - m r \omega^{2} =
m\frac{d^{2}r}{dt^{2}} - \frac{mh^{2}}{r^{3}}

This equation has integration factor \frac{dr}{dt}


\begin{align}
F(r) \, dr
&= F(r) \frac{dr}{dt} \, dt \\
&= m \left(\frac{dr}{dt} \frac{d^{2}r}{dt^{2}} - \frac{h^{2}}{r^{3}} \frac{dr}{dt} \right) \, dt \\
&= \frac m2 \, d\left[\left(\frac{dr}{dt}\right)^2 + \left(\frac hr\right)^2\right]
\end{align}

Integrating yields


\int^{r} F(r) \, dr = \frac m2 \left[\left(\frac{dr}{dt}\right)^2 + \left(\frac hr\right)^2\right]

If h is not zero, the independent variable can be changed from t to ϕ[16]


\frac{d}{dt} = \omega \frac{d}{d\varphi} = \frac{h}{r^{2}} \frac{d}{d\varphi}

giving the new equation of motion[17]


\int^{r} F(r) \, dr = \frac{m h^2}2 \left[\left(-\frac1{r^2} \frac{dr}{d\varphi}\right)^2 + \left(\frac1r\right)^2\right]

Making the change of variables to the inverse radius u = 1/r[17] yields


\left(\frac{du}{d\varphi}\right)^{2} = C - u^2 - G\left(u\right)

 

 

 

 

(1)

where C is a constant of integration and the function G(u) is defined by


G(u) = - \frac2{mh^{2}} \int^{\frac1u} F(r) \, dr

This equation becomes quasilinear on differentiating by ϕ


\frac{d^{2}u}{d\varphi^{2}} + u = -\frac{1}{mh^{2}u^{2}}  F(1/u)

This is known as the Binet equation. Integrating (1) yields the solution for ϕ[18]


\varphi = \varphi_{0} + \int^{\frac1r} \frac{du}{\sqrt{C - u^{2} - G(u)}}

where ϕ0 is another constant of integration. A central-force problem is said to be "integrable" if this final integration can be solved in terms of known functions.

Orbit of the particle[edit]

The total energy of the system Etot equals the sum of the potential energy and the kinetic energy[19]


E_{\mathrm{tot}} = \frac{1}{2} m \dot{r}^{2} + \frac{1}{2} m r^{2} \dot{\varphi}^{2} + U(r) = \frac{1}{2} m \dot{r}^{2} + \frac{m h^{2}}{2 r^{2}} + U(r)

Since the total energy is constant, the rate of change of r can be calculated[20]


\dot{r} = \frac{dr}{dt} = \sqrt{\frac{2}{m}} \sqrt{E_{\mathrm{tot}} - U(r) - \frac{m h^{2}}{2 r^{2}}}

which may be converted (as before) to the derivative of r with respect to the azimuthal angle φ[17]


\frac{dr}{d\varphi} = \frac{r^{2}}{h} \frac{dr}{dt}

Integrating and using the angular-momentum formula L=mh yields the formula[21]


\varphi = \varphi_{0} + \frac{L}{\sqrt{2m}} \int^{r} \frac{dr}{r^{2} \sqrt{E_{\mathrm{tot}} - U(r) - \frac{L^{2}}{2 m r^{2}}}}

which indicates that the angular momentum contributes an effective potential energy[22]


U_{\mathrm{eff}} = U(r) + \frac{L^{2}}{2 m r^{2}}

Changing the variable of integration to the inverse radius yields the integral[23]


\varphi = \varphi_{0} + \int ^{u} \frac{du}{\sqrt{\frac{2m}{L^{2}} E_{\mathrm{tot}} - \frac{2m}{L^{2}} U(1/u) - u^{2}}}

which expresses the above constants C = 2mEtot/L2 and G(u) = 2mU(1/u)/L2 above in terms of the total energy Etot and the potential energy U(r).

Turning points and closed orbits[edit]

Main article: Bertrand's theorem

The rate of change of r is zero whenever the effective potential energy equals the total energy[24]


E_{\mathrm{tot}} = U(r) + \frac{L^{2}}{2 m r^{2}}

The points where this equation is satisfied are known as turning points.[24] The orbit on either side of a turning point is symmetrical; in other words, if the azimuthal angle is defined such that φ = 0 at the turning point, then the orbit is the same in opposite directions, r(φ) = r(−φ).[25]

If there are two turning points such that the radius r is bounded between rmin and rmax, then the motion is contained within an annulus of those radii.[24] As the radius varies from the one turning point to the other, the change in azimuthal angle φ equals[24]


\Delta \varphi = \frac{L}{\sqrt{2m}} \int_{r_{\mathrm{min}}}^{r_{\mathrm{max}}} \frac{dr}{r^{2} \sqrt{E - U(r) - \frac{L^{2}}{2 m r^{2}}}}

The orbit will close upon itself[note 8] provided that Δφ equals a rational fraction of 2π, i.e.,[24]


\Delta \varphi = 2\pi \frac{m}{n}

where m and n are integers. In that case, the radius oscillates exactly m times while the azimuthal angle φ makes exactly n revolutions. In general, however, Δφ will not be such a rational number, and thus the orbit will not be closed. In that case, the particle will eventually pass arbitrarily close to every point within the annulus. Two types of central force always produce closed orbits: F(r) = αr (a linear force) and F(r) = α/r2 (an inverse square law). As shown by Bertrand, these two central forces are the only ones that guarantee closed orbits.[26]

In general, if the angular momentum L is nonzero, the second term prevents the particle from falling into the origin, unless the effective potential energy goes to negative infinity in the limit of r going to zero.[27] Therefore, if there is a single turning point, the orbit generally goes to infinity; the turning point corresponds to a point of minimum radius.

Specific solutions[edit]

Kepler problem[edit]

An animation showing a small particle moving on a red ellipse; a large blue mass is located at one focus of the ellipse.
Classical gravity is a central force. Solving that central-force problem shows that a bound particle follows an elliptical orbit in which equal areas are swept out in equal times, as described by Kepler's second law.

In classical physics, many important forces follow an inverse-square law, such as gravity or electrostatics. The general mathematical form of such inverse-square central forces is


F = \frac{\alpha}{r^{2}} = \alpha u^{2}

for a constant α, which is negative for an attractive force and positive for a repulsive one.

This special case of the classical central-force problem is called the Kepler problem. For an inverse-square force, the Binet equation derived above is linear


\frac{d^{2}u}{d\varphi^{2}} + u = -\frac{\alpha}{mh^{2}}.

The solution of this equation is


u(\varphi) = -\frac{\alpha}{mh^{2}} \left[ 1 - e \cos \left( \varphi - \varphi_{0}\right) \right]

which shows that the orbit is a conic section of eccentricity e; here, φ0 is the initial angle, and the center of force is at the focus of the conic section. Using the half-angle formula for sine, this solution can also be written as


u(\varphi) = u_{1} + (u_{2} - u_{1}) \sin^{2} \left( \frac{\varphi - \varphi_{0}}{2} \right)
Blue ellipse with the two foci indicated as black points. Four line segments go out from the left focus to the ellipse, forming two shaded pseudo-triangles with two straight sides and the third side made from the curved segment of the intervening ellipse.
As for all central forces, the particle in the Kepler problem sweeps out equal areas in equal times, as illustrated by the two blue elliptical sectors. The center of force is located at one of the foci of the elliptical orbit.

where u1 and u2 are constants, with u2 larger than u1. The two versions of the solution are related by the equations


u_{1} + u_{2} = \frac{-2\alpha}{mh^{2}}

and


e = \frac{u_{2} - u_{1}}{u_{2} + u_{1}}

Since the sin2 function is always greater than zero, u2 is the largest possible value of u and the inverse of the smallest possible value of r, i.e., the distance of closest approach (periapsis). Since the radial distance r cannot be a negative number, neither can its inverse u; therefore, u2 must be a positive number. If u1 is also positive, it is the smallest possible value of u, which corresponds to the largest possible value of r, the distance of furthest approach (apoapsis). If u1 is zero or negative, then the smallest possible value of u is zero (the orbit goes to infinity); in this case, the only relevant values of φ are those that make u positive.

For an attractive force (α < 0), the orbit is an ellipse, a hyperbola or parabola, depending on whether u1 is positive, negative, or zero, respectively; this corresponds to an eccentricity e less than one, greater than one, or equal to one. For a repulsive force (α > 0), u1 must be negative, since u2 is positive by definition and their sum is negative; hence, the orbit is a hyperbola. Naturally, if no force is present (α=0), the orbit is a straight line.

Central forces with exact solutions[edit]

The Binet equation for u(φ) can be solved numerically for nearly any central force F(1/u). However, only a handful of forces result in formulae for u in terms of known functions. As derived above, the solution for φ can be expressed as an integral over u


\varphi = \varphi_{0} + \frac{L}{\sqrt{2m}} \int ^{u} \frac{du}{\sqrt{E_{\mathrm{tot}} - U(1/u) - \frac{L^{2}u^{2}}{2m}}}

A central-force problem is said to be "integrable" if this integration can be solved in terms of known functions.

If the force is a power law, i.e., if F(r) = α rn, then u can be expressed in terms of circular functions and/or elliptic functions if n equals 1, -2, -3 (circular functions) and -7, -5, -4, 0, 3, 5, -3/2, -5/2, -1/3, -5/3 and -7/3 (elliptic functions).[28] Similarly, only six possible linear combinations of power laws give solutions in terms of circular and elliptic functions[29][30]


F(r) = Ar^{-3} + Br + Cr^{3} + Dr^{5}

F(r) = Ar^{-3} + Br + Cr^{-5} + Dr^{-7}

F(r) = Ar^{-3} + Br^{-2} + Cr + D

F(r) = Ar^{-3} + Br^{-2} + Cr^{-4} + Dr^{-5}

F(r) = Ar^{-3} + Br^{-2} + Cr^{-3/2} + Dr^{-5/2}

F(r) = Ar^{-3} + Br^{-1/3} + Cr^{-5/3} + Dr^{-7/3}

The following special cases of the first two force types always result in circular functions.


F(r) = Ar^{-3} + Br

F(r) = Ar^{-3} + Br^{-2}

The special case


F(r) = Ar^{-5}

was mentioned by Newton, in corollary 1 to proposition VII of the principia, as the force implied by circular orbits passing through the point of attraction.

Newton's theorem of revolving orbits[edit]

Illustration of Newton's theorem of revolving orbits. The green planet completes one (subharmonic) orbit for every three orbits of the blue planet (k=1/3). A GIF version of this animation is found here.

The term r−3 occurs in all the force laws above, indicating that the addition of the inverse-cube force does not influence the solubility of the problem in terms of known functions. Newton showed that, with adjustments in the initial conditions, the addition of such a force does not affect the radial motion of the particle, but multiplies its angular motion by a constant factor k. An extension of Newton's theorem was discovered in 2000 by Mahomed and Vawda.[30]

Assume that a particle is moving under an arbitrary central force F1(r), and let its radius r and azimuthal angle φ be denoted as r(t) and φ1(t) as a function of time t. Now consider a second particle with the same mass m that shares the same radial motion r(t), but one whose angular speed is k times faster than that of the first particle. In other words, the azimuthal angles of the two particles are related by the equation φ2(t) = k φ1(t). Newton showed that the force acting on the second particle equals the force F1(r) acting on the first particle, plus an inverse-cube central force[31]


F_{2}(r) = F_{1}(r) + \frac{L_{1}^{2}}{mr^{3}} \left( 1 - k^{2} \right)

where L1 is the magnitude of the first particle's angular momentum.

If k2 is greater than one, F2F1 is a negative number; thus, the added inverse-cube force is attractive. Conversely, if k2 is less than one, F2F1 is a positive number; the added inverse-cube force is repulsive. If k is an integer such as 3, the orbit of the second particle is said to be a harmonic of the first particle's orbit; by contrast, if k is the inverse of an integer, such as ⅓, the second orbit is said to be a subharmonic of the first orbit.

Historical development[edit]

Figure 10: Newton's geometrical proof that a moving particle sweeps out equal areas in equal times if and only if the force acting on it at the point B is a central force. Here, the triangle OAB has the same area as the triangles OBC and OBK.

Newton's derivation[edit]

The classical central-force problem was solved geometrically by Isaac Newton in his Philosophiæ Naturalis Principia Mathematica, in which Newton introduced his laws of motion. Newton used an equivalent of leapfrog integration to convert the continuous motion to a discrete one, so that geometrical methods may be applied. In this approach, the position of the particle is considered only at evenly spaced time points. For illustration, the particle in Figure 10 is located at point A at time t = 0, at point B at time t = Δt, at point C at time t = 2Δt, and so on for all times t = nΔt, where n is an integer. The velocity is assumed to be constant between these time points. Thus, the vector rAB = rB − rA equals Δt times the velocity vector vAB (red line), whereas rBC = rC − rB equals vBCΔt (blue line). Since the velocity is constant between points, the force is assumed to act instantaneously at each new position; for example, the force acting on the particle at point B instantly changes the velocity from vAB to vBC. The difference vector Δr = rBC − rAB equals ΔvΔt (green line), where Δv = vBC − vAB is the change in velocity resulting from the force at point B. Since the acceleration a is parallel to Δv and since F = ma, the force F must be parallel to Δv and Δr. If F is a central force, it must be parallel to the vector rB from the center O to the point B (dashed green line); in that case, Δr is also parallel to rB.

If no force acts at point B, the velocity is unchanged, and the particle arrives at point K at time t = 2Δt. The areas of the triangles OAB and OBK are equal, because they share the same base (rAB) and height (r). If Δr is parallel to rB, the triangles OBK and OBC are likewise equal, because they share the same base (rB) and the height is unchanged. In that case, the areas of the triangles OAB and OBC are the same, and the particle sweeps out equal areas in equal time. Conversely, if the areas of all such triangles are equal, then Δr must be parallel to rB, from which it follows that F is a central force. Thus, a particle sweeps out equal areas in equal times if and only if F is a central force.

Alternative derivations of the equations of motion[edit]

Lagrangian mechanics[edit]

The formula for the radial force may also be obtained using Lagrangian mechanics. In polar coordinates, the Lagrangian L of a single particle in a potential energy field U(r) is given by


L = \frac{1}{2} m \dot{r}^{2} + \frac{1}{2} m r^{2} \dot{\varphi}^{2} - U(r)

Then Lagrange's equations of motion


\frac{d}{dt} \left( \frac{\partial L}{\partial \dot{r}} \right) = \frac{\partial L}{\partial r}

take the form


m\ddot{r} = m r \dot{\varphi}^{2} - \frac{dU}{dr} = \frac{m h^{2}}{r^{3}} \dot{\varphi} + F(r)

since the magnitude F(r) of the radial force equals the negative derivative of the potential energy U(r) in the radial direction.

Hamiltonian mechanics[edit]

The radial force formula may also be derived using Hamiltonian mechanics. In polar coordinates, the Hamiltonian can be written as


H = \frac{1}{2m} \left( p_{r}^{2} + \frac{p_{\phi}^{2}}{r^{2}} \right) + U(r)

Since the azimuthal angle φ does not appear in the Hamiltonian, its conjugate momentum pφ is a constant of the motion. This conjugate momentum is the magnitude L of the angular momentum, as shown by the Hamiltonian equation of motion for φ


\frac{d\varphi}{dt} = \frac{\partial H}{\partial p_{\varphi}} = \frac{p_{\varphi}}{mr^{2}} = \frac{L}{mr^{2}}

The corresponding equation of motion for r is


\frac{dr}{dt} = \frac{\partial H}{\partial p_{r}} = \frac{p_{r}}{m}

Taking the second derivative of r with respect to time and using Hamilton's equation of motion for pr yields the radial-force equation


\frac{d^{2}r}{dt^{2}} = \frac{1}{m} \frac{dp_{r}}{dt} = -\frac{1}{m} \left( \frac{\partial H}{\partial r} \right) = \frac{p_{\varphi}^{2}}{m^{2} r^{3}} - \frac{1}{m} \frac{dU}{dr} = \frac{L^{2}}{m^{2} r^{3}} + \frac{1}{m} F(r)

Hamilton-Jacobi equation[edit]

The orbital equation can be derived directly from the Hamilton-Jacobi equation.[32] Adopting the radial distance r and the azimuthal angle φ as the coordinates, the Hamilton-Jacobi equation for a central-force problem can be written


\frac{1}{2m} \left( \frac{dS_{r}}{dr} \right)^{2} + 
\frac{1}{2m r^{2}} \left( \frac{dS_{\varphi}}{d\varphi} \right)^{2} + U(r) = E_{\mathrm{tot}}

where S = Sφ(φ) + Sr(r) - Etott is Hamilton's principal function, and Etot and t represent the total energy and time, respectively. This equation may be solved by successive integrations of ordinary differential equations, beginning with the φ equation


\frac{dS_{\varphi}}{d\varphi} = p_{\varphi} = L

where pφ is a constant of the motion equal to the magnitude of the angular momentum L. Thus, Sφ(φ) = Lφ and the Hamilton–Jacobi equation becomes


\frac{1}{2m} \left( \frac{dS_{r}}{dr} \right)^{2} + 
\frac{L^{2}}{2m r^{2}} + U(r) = E_{\mathrm{tot}}

Integrating this equation for Sr yields


S_{r} (r) = \sqrt{2m} \int dr \sqrt{E_{\mathrm{tot}} - U(r) -  \frac{L^{2}}{2m r^{2}}}

Taking the derivative of S with respect to L yields the orbital equation derived above


\varphi_{0} = \frac{\partial S}{\partial L} = \frac{\partial S_{\varphi}}{\partial L} + \frac{\partial S_{r}}{\partial L} = \varphi - \frac{L}{\sqrt{2m}} \int^{r} \frac{dr}{r^{2} \sqrt{E_{\mathrm{tot}} - U(r) - \frac{L^{2}}{2m r^{2}}}}

See also[edit]

Notes[edit]

  1. ^ Throughout this article, boldface type is used to indicate that quantities such as r and F are vectors, whereas ordinary numbers are written in italics. Briefly, a vector v is a quantity that has a magnitude v (also written |v|) and a direction. Vectors are often specified by their components. For example, the position vector r = (x, y) in Cartesian coordinates is described as an ordered pair of its x and y coordinates.
  2. ^ In this article, Newton's notation for derivatives ("dot notation") is used sometimes to make the formulae easier to read; it has no other significance. In this notation, a single dot over a variable signifies its first derivative with respect to time, e.g.,
    
\dot{r} = \frac{dr}{dt}
    Similarly, a double dot over a variable signifies its second derivative with respect for time, e.g.,
    
\ddot{r} = \frac{d^{2}r}{dt^{2}}
  3. ^ Here, the times symbol × indicates the vector cross product, not simple multiplication.
  4. ^ If a and b are three-dimensional vectors, their vector cross product c = a × b is always perpendicular to the plane defined by a and b.
  5. ^ This formula for the azimuthal unit vector may be verified by calculation; its magnitude equals one
    
\hat{\boldsymbol\varphi} \cdot \hat{\boldsymbol\varphi} = (-\sin \varphi )^{2} + (\cos \varphi)^{2} = 1
    and its dot-product with r equals zero
    
\hat{\boldsymbol\varphi} \cdot \mathbf{\hat{r}}  = -\sin \varphi \cos \varphi + \cos \varphi \sin \varphi = 0
    Therefore, it is a unit vector perpendicular to the radial vector r.
  6. ^ The area of a triangle equals one half the base times its height. In this case, the base is given by vΔt and the height equals the impact parameter r.
  7. ^ A parallel-force problem is one in which the force is exactly zero along one direction.
  8. ^ A closed orbit is one that returns to its starting position after a finite time with exactly the same velocity. Hence, it executes exactly the same motion over and over again.

References[edit]

  1. ^ Goldstein, p. 71; Landau and Lifshitz, p. 30; Sommerfeld, p. 39; Symon, p. 121.
  2. ^ Landau and Lifshitz, p. 30; Symon, p. 121.
  3. ^ Goldstein, p. 4; Landau and Lifshitz, p. 30; Symon, p. 122.
  4. ^ Goldstein, p. 71; Landau and Lifshitz, p. 30; Whittaker, p. 77.
  5. ^ Sommerfeld, p. 39; Symon, p. 123.
  6. ^ Goldstein, pp. 70–71; Landau and Lifshitz, p. 29; Symon, pp. 182–185; Whittaker, pp. 76–77.
  7. ^ Goldstein, p. 72; Landau and Lifshitz, p. 30; Whittaker, p. 77.
  8. ^ Goldstein, pp. 2–3, 6–7.
  9. ^ a b Goldstein, p. 72.
  10. ^ Goldstein, p. 73; Landau and Lifshitz, pp. 30–31; Sommerfeld, pp. 39–40; Symon, pp. 124, 127.
  11. ^ Landau and Lifshitz, p. 31.
  12. ^ Goldstein, p. 73; Landau and Lifshitz, pp. 30–31; Sommerfeld, pp. 36, 39; Symon, pp. 127–128.
  13. ^ Goldstein, p. 73; Landau and Lifshitz, p. 31; Sommerfeld, p. 39; Symon, p. 135.
  14. ^ Whittaker, pp. 93–94.
  15. ^ Goldstein, p. 73.
  16. ^ Goldstein, p. 75, 86.
  17. ^ a b c Goldstein, p. 86.
  18. ^ Whittaker, pp. 80‒81.
  19. ^ Goldstein, p. 4.
  20. ^ Goldstein, p. 75.
  21. ^ Goldstein, p. 87.
  22. ^ Goldstein, pp. 76–82.
  23. ^ Goldstein, p. 88.
  24. ^ a b c d e Landau and Lifshitz, p. 32.
  25. ^ Landau and Lifshitz, pp. 32–33.
  26. ^ Goldstein, pp. 601–605.
  27. ^ Landau and Lifshitz, p. 33.
  28. ^ Whittaker, pp. 80–95.
  29. ^ Broucke R (1980). "Notes on the central force rn". Astrophysics and Space Sciences 72: 33–53. Bibcode:1980Ap&SS..72...33B. doi:10.1007/BF00642162. 
  30. ^ a b Mahomed FM, Vawda F (2000). "Application of Symmetries to Central Force Problems". Nonlinear Dynamics 21: 307–315. doi:10.1023/A:1008317327402. 
  31. ^ Newton, Principia, section IX of Book I, Propositions 43–45, pp. 135–147.
  32. ^ Goldstein, pp. 454–457; Landau and Lifshitz, pp. 149–151; Misner, Thorne, and Wheeler, pp. 644–649; Sommerfeld, pp. 235–238.

Bibliography[edit]

  • Symon KR (1971). Mechanics (3rd ed.). Reading, MA: Addison-Wesley. ISBN 0-201-07392-7. 
  • Whittaker ET (1937). A Treatise on the Analytical Dynamics of Particles and Rigid Bodies, with an Introduction to the Problem of Three Bodies (4th ed.). New York: Dover Publications. ISBN 978-0-521-35883-5. 

External links[edit]