Bertrand's theorem

In classical mechanics, Bertrand's theorem states that among central-force potentials with bound orbits, there are only two types of central-force (radial) scalar potentials with the property that all bound orbits are also closed orbits.[1][2]

Joseph Bertrand

The first such potential is an inverse-square central force such as the gravitational or electrostatic potential:

${\displaystyle V(r)=-{\frac {k}{r}}}$ arising from force ${\displaystyle f(r)=-{\frac {dV}{dr}}=-{\frac {k}{r^{2}}}}$.

The second is the radial harmonic oscillator potential:

${\displaystyle V(r)={\frac {1}{2}}kr^{2}}$ with force ${\displaystyle f(r)=-{\frac {dV}{dr}}=-kr}$.

The theorem is named after its discoverer, Joseph Bertrand.

Description

Small changes in the power of the force scaling with distance will lead to significantly different kind of orbits.

All attractive central forces can produce circular orbits, which are naturally closed orbits. The only requirement is that the central force exactly equals the centripetal force, which determines the required angular velocity for a given circular radius. Non-central forces (i.e., those that depend on the angular variables as well as the radius) are ignored here, since they do not produce circular orbits in general.

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

${\displaystyle m{\frac {d^{2}r}{dt^{2}}}-mr\omega ^{2}=m{\frac {d^{2}r}{dt^{2}}}-{\frac {L^{2}}{mr^{3}}}=-{\frac {dV}{dr}},}$

where ${\displaystyle \omega \equiv {\frac {d\theta }{dt}}}$, and the angular momentum L = mr²ω is conserved. For illustration, the first term on the left is zero for circular orbits, and the applied inwards force ${\displaystyle {\frac {dV}{dr}}}$ equals the centripetal force requirement mrω², as expected.

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

${\displaystyle {\frac {d}{dt}}={\frac {L}{mr^{2}}}{\frac {d}{d\theta }},}$

giving the new equation of motion that is independent of time:

${\displaystyle {\frac {L}{r^{2}}}{\frac {d}{d\theta }}\left({\frac {L}{mr^{2}}}{\frac {dr}{d\theta }}\right)-{\frac {L^{2}}{mr^{3}}}=-{\frac {dV}{dr}}.}$

This equation becomes quasilinear on making the change of variables ${\displaystyle u\equiv {\frac {1}{r}}}$ and multiplying both sides by ${\displaystyle {\frac {mr^{2}}{L^{2}}}}$ (see also Binet equation):

${\displaystyle {\frac {d^{2}u}{d\theta ^{2}}}+u=-{\frac {m}{L^{2}}}{\frac {d}{du}}V\left({\frac {1}{u}}\right).}$

As noted above, all central forces can produce circular orbits given an appropriate initial velocity. However, if some radial velocity is introduced, these orbits need not be stable (i.e., remain in orbit indefinitely) nor closed (repeatedly returning to exactly the same path). Here we show that stable, exactly closed orbits can be produced only with an inverse-square force or radial harmonic oscillator potential (a necessary condition). In the following sections, we show that those force laws do produce stable, exactly closed orbits (a sufficient condition).

Define J(u) as

${\displaystyle {\frac {d^{2}u}{d\theta ^{2}}}+u=J(u)\equiv -{\frac {m}{L^{2}}}{\frac {d}{du}}V\left({\frac {1}{u}}\right)=-{\frac {m}{L^{2}u^{2}}}f\left({\frac {1}{u}}\right),}$

where f represents the radial force. The criterion for perfectly circular motion at a radius r₀ is that the first term on the left be zero:

${\displaystyle u_{0}=J(u_{0})=-{\frac {m}{L^{2}u_{0}^{2}}}f\left({\frac {1}{u_{0}}}\right),}$

(1)

where ${\displaystyle u_{0}\equiv 1/r_{0}}$.

The next step is to consider the equation for u under small perturbations ${\displaystyle \eta \equiv u-u_{0}}$ from perfectly circular orbits. On the right, the J function can be expanded in a standard Taylor series:

${\displaystyle J(u)\approx J(u_{0})+\eta J'(u_{0})+{\frac {1}{2}}\eta ^{2}J''(u_{0})+{\frac {1}{6}}\eta ^{3}J'''(u_{0})+\cdots }$

Substituting this expansion into the equation for u and subtracting the constant terms yields

${\displaystyle {\frac {d^{2}\eta }{d\theta ^{2}}}+\eta =\eta J'(u_{0})+{\frac {1}{2}}\eta ^{2}J''(u_{0})+{\frac {1}{6}}\eta ^{3}J'''(u_{0})+\cdots ,}$

which can be written as

${\displaystyle {\frac {d^{2}\eta }{d\theta ^{2}}}+\beta ^{2}\eta ={\frac {1}{2}}\eta ^{2}J''(u_{0})+{\frac {1}{6}}\eta ^{3}J'''(u_{0})+\cdots ,}$

(2)

where ${\displaystyle \beta ^{2}\equiv 1-J'(u_{0})}$ is a constant. β² must be non-negative; otherwise, the radius of the orbit would vary exponentially away from its initial radius. (The solution β = 0 corresponds to a perfectly circular orbit.) If the right side may be neglected (i.e., for small perturbations), the solutions are

${\displaystyle \eta (\theta )=h_{1}\cos(\beta \theta ),}$

where the amplitude h₁ is a constant of integration. For the orbits to be closed, β must be a rational number. What's more, it must be the same rational number for all radii, since β cannot change continuously; the rational numbers are totally disconnected from one another. Using the definition of J along with equation (1),

${\displaystyle J'(u_{0})={\frac {2}{u_{0}}}\left[{\frac {m}{L^{2}u_{0}^{2}}}f\left({\frac {1}{u_{0}}}\right)\right]-\left[{\frac {m}{L^{2}u_{0}^{2}}}f\left({\frac {1}{u_{0}}}\right)\right]{\frac {1}{f\left({\frac {1}{u_{0}}}\right)}}{\frac {df}{du}}=-2+{\frac {u_{0}}{f\left({\frac {1}{u_{0}}}\right)}}{\frac {df}{du}}=1-\beta ^{2},}$

where ${\displaystyle {\frac {df}{du}}}$ is evaluated at ${\displaystyle 1/u_{0}}$. Since this must hold for any value of u₀,

${\displaystyle {\frac {df}{dr}}=(\beta ^{2}-3){\frac {f}{r}},}$

which implies that the force must follow a power law

${\displaystyle f(r)=-{\frac {k}{r^{3-\beta ^{2}}}}.}$

Hence, J must have the general form

${\displaystyle J(u)={\frac {mk}{L^{2}}}u^{1-\beta ^{2}}.}$

(3)

For more general deviations from circularity (i.e., when we cannot neglect the higher-order terms in the Taylor expansion of J), η may be expanded in a Fourier series, e.g.,

${\displaystyle \eta (\theta )=h_{0}+h_{1}\cos \beta \theta +h_{2}\cos 2\beta \theta +h_{3}\cos 3\beta \theta +\cdots }$

We substitute this into equation (2) and equate the coefficients belonging to the same frequency, keeping only the lowest-order terms. As we show below, h₀ and h₂ are smaller than h₁, being of order ${\displaystyle h_{1}^{2}}$. h₃, and all further coefficients, are at least of order ${\displaystyle h_{1}^{3}}$. This makes sense, since ${\displaystyle h_{0},h_{2},h_{3},\ldots }$ must all vanish faster than h₁ as a circular orbit is approached.

${\displaystyle h_{0}=h_{1}^{2}{\frac {J''(u_{0})}{4\beta ^{2}}},}$

${\displaystyle h_{2}=-h_{1}^{2}{\frac {J''(u_{0})}{12\beta ^{2}}},}$

${\displaystyle h_{3}=-{\frac {1}{8\beta ^{2}}}\left[h_{1}h_{2}{\frac {J''(u_{0})}{2}}+h_{1}^{3}{\frac {J'''(u_{0})}{24}}\right].}$

From the cos(βθ) term, we get

${\displaystyle 0=(2h_{1}h_{0}+h_{1}h_{2}){\frac {J''(u_{0})}{2}}+h_{1}^{3}{\frac {J'''(u_{0})}{8}}={\frac {h_{1}^{3}}{24\beta ^{2}}}\left(3\beta ^{2}J'''(u_{0})+5J''(u_{0})^{2}\right),}$

where in the last step we substituted in the values of h₀ and h₂.

Using equations (3) and (1), we can calculate the second and third derivatives of J evaluated at u₀:

${\displaystyle J''(u_{0})=-{\frac {\beta ^{2}(1-\beta ^{2})}{u_{0}}},}$

${\displaystyle J'''(u_{0})={\frac {\beta ^{2}(1-\beta ^{2})(1+\beta ^{2})}{u_{0}^{2}}}.}$

Substituting these values into the last equation yields the main result of Bertrand's theorem:

${\displaystyle \beta ^{2}(1-\beta ^{2})(4-\beta ^{2})=0.}$

Hence, the only potentials that can produce stable closed non-circular orbits are the inverse-square force law (β = 1) and the radial harmonic-oscillator potential (β = 2). The solution β = 0 corresponds to perfectly circular orbits, as noted above.

Classical field potentials

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

${\displaystyle V(\mathbf {r} )={\frac {-k}{r}}=-ku.}$

The orbit u(θ) can be derived from the general equation

${\displaystyle {\frac {d^{2}u}{d\theta ^{2}}}+u=-{\frac {m}{L^{2}}}{\frac {d}{du}}V\left({\frac {1}{u}}\right)={\frac {km}{L^{2}}},}$

whose solution is the constant ${\displaystyle {\frac {km}{L^{2}}}}$ plus a simple sinusoid:

${\displaystyle u\equiv {\frac {1}{r}}={\frac {km}{L^{2}}}[1+e\cos(\theta -\theta _{0})],}$

where e (the eccentricity), and θ₀ (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 (see Laplace–Runge–Lenz vector):

${\displaystyle e={\sqrt {1+{\frac {2EL^{2}}{k^{2}m}}}}.}$

Comparing these formulae shows that E < 0 corresponds to an ellipse, E = 0 corresponds to a parabola, and E > 0 corresponds to a hyperbola. In particular, ${\displaystyle E=-{\frac {k^{2}m}{2L^{2}}}}$ for perfectly circular orbits.

Harmonic oscillator

To solve for the orbit under a radial harmonic-oscillator potential, it's easier to work in components r = (x, y, z). The potential can be written as

${\displaystyle V(\mathbf {r} )={\frac {1}{2}}kr^{2}={\frac {1}{2}}k(x^{2}+y^{2}+z^{2}).}$

The equation of motion for a particle of mass m is given by three independent Euler equations:

${\displaystyle {\frac {d^{2}x}{dt^{2}}}+\omega _{0}^{2}x=0,}$

${\displaystyle {\frac {d^{2}y}{dt^{2}}}+\omega _{0}^{2}y=0,}$

${\displaystyle {\frac {d^{2}z}{dt^{2}}}+\omega _{0}^{2}z=0,}$

where the constant ${\displaystyle \omega _{0}^{2}\equiv {\frac {k}{m}}}$ must be positive (i.e., k > 0) to ensure bounded, closed orbits; otherwise, the particle will fly off to infinity. The solutions of these simple harmonic oscillator equations are all similar:

${\displaystyle x=A_{x}\cos(\omega _{0}t+\phi _{x}),}$

${\displaystyle y=A_{y}\cos(\omega _{0}t+\phi _{y}),}$

${\displaystyle z=A_{z}\cos(\omega _{0}t+\phi _{z}),}$

where the positive constants A_x, A_y and A_z represent the amplitudes of the oscillations, and the angles φ_x, φ_y and φ_z represent their phases. The resulting orbit r(t) = [x(t), y(y), z(t)] is closed because it repeats exactly after a period

${\displaystyle T\equiv {\frac {2\pi }{\omega _{0}}}.}$

The system is also stable because small perturbations in the amplitudes and phases cause correspondingly small changes in the overall orbit.

References

1. Bertrand J (1873). "Théorème relatif au mouvement d'un point attiré vers un centre fixe". C. R. Acad. Sci. 77: 849–853.
2. Johnson, Porter Wear (2010-02-24). Classical Mechanics With Applications. World Scientific. pp. 149–. ISBN 9789814304153. Retrieved 2 December 2012.

Further reading

• Goldstein, H. (1980). Classical Mechanics (2nd ed.). Addison-Wesley. ISBN 978-0-201-02918-5.
• Santos, F. C.; Soares, V.; Tort, A. C. (2011). "An English translation of Bertrand's theorem". Latin American Journal of Physics Education. 5 (4): 694–696. arXiv:0704.2396. Bibcode:2007arXiv0704.2396S.