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I saw a question a few days ago which referred to Bertrand's theorem. So, I now know that stable, closed orbits only occur when the potential function is $\frac{-k}{r}$ or $\tfrac{1}{2}kr^2$.

  1. If we relax the conditions to stable but not necessarily closed orbits then what are the possibilities?
  2. If we restrict consideration to power law forces $kr^n$, for what $n$ are stable orbits possible?

My memory was that for $n \geq -2$ there are stable orbits but for $n \leq -3$ there are not. I forget the cases between $-2$ and $-3$.

I believe that a circular orbit is possible for all $n$ but consider a slight perturbation to that orbit. For the well known $n = -2$ case, we will get a ellipse with low eccentricity. If my memory is right then for $n = -1$, the orbit will be stable just not closed. For $n = -3$, the orbit will not be stable and spiral in or out after the perturbation.

Am I right on the power law forces?

I have tried searching here and elsewhere but failed to find my answer.

Clarification: note that I am not interested only in circular orbits. The primary question is whether they are stable if perturbed but further information on the nature of stable orbits for central forces would be very welcome.

Diracology
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badjohn
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  • If I remember correctly, stable circular orbits only exists if $n(n+2)\ge 0$. –  Jul 03 '17 at 10:21
  • Related to On the Stability of Circular Orbits – sammy gerbil Jul 03 '17 at 10:25
  • @sammygerbil Thank you. That was helpful. It seems that my memory was close but that has confirmed it and answered the case between $-2$ and $-3$. – badjohn Jul 03 '17 at 10:32
  • @LucJ.Bourhis The answer quoted by Sammy does not seem to fit your condition. Your condition seems to allow $-3$ but not $-1$. – badjohn Jul 03 '17 at 10:33
  • I did remember only half of the story indeed. A quick back of the envelope calculation gives either $k r^n$ with $n>0$ or $-kr^{-n}$ with $0<n<2$, and $k>0$ in both cases. As the condition for stable circular orbits I mean. –  Jul 03 '17 at 10:43
  • @LucJ.Bourhis Thanks. However, I am not only interested in circular orbits. – badjohn Jul 03 '17 at 10:55
  • Yes, I understand. I do not know a reference either but it seems to me the best avenue would be to use the usual Clairaut-Binet trick: $x=L/mr$ where $L$ is the angular momentum, and then get a differential equation $m d^2x/d\phi = -V'(x)$ where $\phi$ is the usual polar angle. The result you seek is then whether all solutions are bounded below by some $x_m>0$ and above by some finite $x_M$, both depending on $L$ I presume. –  Jul 03 '17 at 11:02
  • This old post may be helpful. An intuitive proof of Bertrand's theorem https://physics.stackexchange.com/q/110123/37364 – mmesser314 Jul 03 '17 at 13:34
  • @mmesser314 Thanks. I have seen some proofs of Bertrand's Theorem but I am asking about a different case: where the orbit is stable but not necessarily closed. – badjohn Jul 03 '17 at 13:44

2 Answers2

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This isn't going to be a rigorous treatment, but you can get an idea of what is going on by considering the effective potential of the orbiting body. If we consider a frame that is corotating with the body then in this frame there is a fictitious centrifugal force pushing the body outwards, and associated with this force there is a potential $L^2/2mr^2$ where $L$ is the (constant) angular momentum. Adding this to the gravitational potential $U(r)$ gives an effective potential:

$$ V_\text{eff} = \frac{L^2}{2mr^2} + U(r) $$

If we take $U(r) = -k/r$ then we get an effective potential looking something like:

Effective potential

If it's a bound orbit this potential always has a minimum. This exists because if the orbiting object approaches the central mass the positive $r^{-2}$ term dominates and pushes it out again, while if the object moves to large $r$ the negative $r^{-1}$ term pulls it in again. Effective the particle oscillates around the minimum of the effective potential so its orbit is always stable.

The problem is that with different gravitational potentials we don't get this stable minimum. For example if $U(r) = -kr^{-2}$ the effective potential is just $\pm Ar^{-2}$ for some constant $A$. With the plus sign the potential always pushes the orbiting object outwards to infinity and with the minus sign the potential pulls it inwards to crash into the central body.

Move to $U(r) = -kr^{-3}$, or any $-kr^{-n}$ for $n \ge 3$, and now we get only a maximum like:

Effective potential

So again any perturbation sends the orbiting object outward to infinity or inwards to crash into the object.

The special feature of the $-kr^{-1}$ potential is that it falls more slowly with distance than the $r^{-2}$ potential due to the fictitious force. That's why only it give a stable orbit. If you allow non-integral powers then any $n \lt 2$ also gives a stable orbit, though we normally consider only integral values of $n$.

John Rennie
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  • Thanks. Integral values are of most interest; the others are just a mathematical curiosity. Are you considering only the negative cases? Bertrand's Theorem gives us one more case with not just stable but closed orbits. Your use of $n$ seems to be different to mine. Your positive $n$ is my negative. – badjohn Jul 03 '17 at 12:38
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Not every central force admits a circular orbit since only an attractive interaction can balance the repulsive centrifugal term. On the other hand, every attractive force has a circular orbit since by an appropriate choice of angular momentum the centrifugal term, $L^2/2\mu r^2$, can be chosen to cancel the attractive interaction, $U(r)$. Finally, attractive potential is not a sufficient for the existence of stable orbits.

The circular orbit of radius $r_0$ is stable if and only if $U_{\mathrm{eff}}(r_0)$ corresponds to a minimum of the effective potential, $$U_{\mathrm{eff}}(r)=\frac{L^2}{2\mu r^2}+U(r).$$ This implies that the second derivative of $U_{\mathrm{eff}}$ at $r_0$ must be positive. Hence, $$U''(r_0)>-\frac{3L^2}{\mu r_0^4}.\tag1$$

For circular orbits, the radial effective force (which includes interaction and centrifugal forces) vanishes and then $U_{\mathrm{eff}}(r_0)'=0$. Thus $$r_0^3=\frac{L^2}{\mu U'(r_0)}.$$ Plugging this into Eqn (1) we obtain the following condition $$\frac{U''(r_0)}{U'(r_0)}+\frac{3}{r_0}>0,$$ for stable orbits. As an example, assuming an attractive potential with a power law $U=kr^{n}$, the last equation gives us that is has stable orbits only for $n>-2$.

It is worth mentioning that there are different concepts of stability regarding orbital motion. The one assumed here, for which the above result holds, says that a circular orbit is stable if it remains bounded under small perturbations (a bounded orbit is one whose radius is limited by $r_{\mathrm{min}}\leq r\leq r_{\mathrm{max}}$). A different and also common concept is Lyapunov Stability. In this case, among all power law central forces, only the harmonic oscillator gives stable orbits.

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