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## 12.1. Celestial Mechanics

Alice: You know, we really should be able to derive the orbital period analytically. Let me try to remember my celestial mechanics. I remember that there was one equation that had no factors of or whatever in it. Ah yes,

Here is the semi-major axis, is the angular frequency of the motion, in other words the period of the orbit is given in terms of as .

Bob: That's a handy formula to remember. What does that give in our case? We started with and took but what was our initial value for ?

Alice: We'll have to reconstruct that. It must be larger than 0.5, but not much larger. At the time of pericenter the particles were much closer than at apocenter, which means that the eccentricity was fairly large, and the apocenter distance not much smaller than .

I remember another handy formula: the total energy in a two-body system is equal to

That is easy to remember, since the virial theorem tells you that the potential energy is twice as large as the kinetic energy, on average, and therefore the total energy is half the potential energy, also on average. Now in a Kepler orbit, it turns out that the average of happens to be .

Bob: I can see that it is useful to remember those qualitative facts. That is easier than trying to remember factors of 3 or 4 in formulas that you learn by heart and than later half forget.

Alice: Yes, the only numbers I like are 1 and 0 and infinity. So let us determine the total energy, and then we now our semi-major axis .

Bob: But we have that already: according to the output of my program it is E_tot = -0.875, initially. In other words, .

Alice: Inverting my previous equation, we get

With , we get

So with your value , that gives us . But hey, that can't be right. It should be larger than 0.5, since the maximum distance between two particles in any Kepler orbit is , and we started at a distance of unity!

Bob: That is puzzling. But you just stepped through my code. You were so happy with the clarity of the statements like etot = ekin + epot.

Alice: Let's do an independent check. This is like debugging, but now on the level of the physics, rather than the numerics. Let me just use pen and paper to determine the initial total energy. Here are the equations:

with and , right?

Bob: Right. And these are velocities in the center of mass frame of the two particles. These are equal in magnitude but opposite in direction, so each one is one half of the relative velocity. The original relative velocity was 1/2, so each of the two is 1/4, and . Let's do it very carefully, to make sure we don't drop some factor somewhere. We have now for the initial total energy:

Alice: That is exactly four times smaller than the value that your program gave us. And it would imply a semi-major axis of

Now that is a much more reasonable number! Just as I had predicted: larger than 0.5, but not much larger. Look:

```    |gravity> bc -lq
4/7
.57142857142857142857
```
This has to be correct. We did it from first principles, little step for little step, and the result is just what was expected.

## 12.2. The Role of the Masses

Bob: If this is right, then the question is what went wrong with my program? I agree that a value of is unphysical. But like I said, you just checked with me every statement in the code!

Alice: Well, your calculation can't be all wrong. You had the factor 7 in the denominator, that's unlikely to come out correctly by chance. You were off by a factor 4. I think there must be something wrong with your units.

Bob: My units??? You saw as well as I did that I used , and there were no other scaling units involved. We gave each particle a mass of 0.5, with a total mass of 1.0, which went into the Body description for the relative motion of the two particles.

Hey, wait a minute. We use a mass of 1 for our relative particle and a mass of 0.5 for each individual particle. There is a factor two between them, and two times two makes four.

Alice: Indeed, the factor four that your program was off with. And I think you found the solution, or at least the direction of the solution. Look, in your code you use the correct scaling for kinetic and potential energy, but you don't have any mass factors in there.

Bob: Perhaps I was thinking about the fact that we started with a total mass of one, or perhaps I just forgot. Can we correct that? The potential energy is

For our case, , so neglecting the mass factors, I have overestimated the potential energy by a factor of four. The kinetic energy is

In our equal mass case, the two velocities in the center of mass are each exactly half of the relative velocity, so their squares are four times smaller. The masses sum up to unity, so yes, I have overestimated the kinetic energy by the exact same value of four.

Alice: Problem solved.

Bob: Still, I wonder, I thought I had done something similar in another code, quite a while ago, and I think I did give that one considerable thought. The question is, should I do my energy diagnostics in the center of mass frame, or is there a way to save my current code?

What I mean is that the whole two-body problem is specified in terms of relative positions and relative velocities and the sum of the masses. In the equations of motions, nowhere do the individual velocities in the center of mass frame come in, nor do the individual masses appear. That makes me think that my mistake might not have been that bad after all. Could it be that I am always off by a constant factor, or at least by the same factor in potential and kinetic energy, so that it still makes sense to add the two and thus check for energy conservation?

Alice: What we have to do is to check how the reduced mass comes in.

Bob: Ah yes, that rings a bell, from my celestial mechanics class. The relative motion of two bodies under the influence of gravity, or of electrostatic forces for that matter, can be described by the equivalent motion of a pseudo-particle with a different mass, the reduced mass. But how did that go? We can look in any old celestial mechanics book, but it would be more fun to try to reconstruct it ourselves.

## 12.3. Reduced Mass

Alice: It can't be that hard. The potential energy is already given in terms of relative coordinates, also in the center-of-mass frame. It is

What we have to do now is to rewrite the kinetic energy in relative coordinates. We know that in the center-of-mass frame the following lever-like relations hold:

where is still the relative velocity between the two particles.

This gives us for the total kinetic energy, in the center of mass frame:

The total energy can thus be written as

You were right about the reduced mass: this is defined for two particles as:

It has the physical dimensions of mass, and for a light particle in orbit around a heavy particle, it reduces to the mass of the light particle. If , for example, , to within about ten percent the same as the mass of the light particle. Most of the relative motion also occurs in the motion of the light particle, so in the limit that the mass ratio grows even much larger, the relative motion becomes effectively that of the light particle around a fixed center of attraction.

Bob: And I can see now what I have done in my code: I have given the kinetic and potential energy per unit reduced mass. And I remember now why I have done that before, several years ago: there I had chosen units in which the total mass of the two-body system was unity. In that case what I did would have been correct. But now I should go back and include the factor to my potential energy. If in the future we or someone else will use our code for a case where the sum of the masses is not unity, the code as it is will give a wrong answer.

I will rewrite the relevant code right away as follows:

```  def ekin                        # kinetic energy
@ek = 0.5*(@vel*@vel)         # per unit of reduced mass
end

def epot                        # potential energy
@ep = -@mass/sqrt(@pos*@pos)  # per unit of reduced mass
end

def e_init                      # initial total energy
@e0 = ekin + epot             # per unit of reduced mass
end
```
Alice: I'm glad we checked not only that the code ran correctly, but that we had the right conversions between physical formula and expressions in the code.

Bob: Yes, this is something students always get entangled with when they start coding something themselves, and I can't really blame them, since I'm still making similar mistakes myself.

Alice: The nice thing about getting more experience is not so much that you stop making errors, it is more that you get better at spotting them, and then figuring out where they come from, what the wrong assumptions were that led you to the error in the first place. Once you are that far, correcting the error is generally quite simple.

## 12.4. Wrapping It Up

Bob: I think we have now collected enough material to get my students going for quite a while.

Alice: Shall we wrap it up, and write up what we have learned?

Bob: Yes, we can do that, but I have one worry. We are both quite happy with what we have learned now about Ruby, but there remains the fact that we cannot yet complete a simple Kepler orbit at reasonable precision without sitting here in front of our terminals, twiddling our thumbs waiting for the computer to return an answer. This will give people a bad impression about Ruby as being too slow for numerical applications.

Alice: You said that you can probably speed up the Ruby programs by two orders of magnitude.

Bob: I will try to do that soon, but I think I have a better idea. Our last program has become so structured now, that I think it will be easy to generalize it to higher order integrators, such as the second-order leapfrog, or even fourth order integrators. That should speed up our Kepler orbits quite a bit, and also help us to get beyond the single-precision level we are currently stuck with.

Alice: If you think you can do that with only minor modifications, that would be great, but I don't think you should start a whole new project. We should round off our current part, and present that to the students. We can learn from their reactions what is and is not clear, and then we can see better what to do next.

Bob: Yeah, I know, I have a tendency to just keep going on and on when I have fun tinkering with things. Okay, I promise you: I'll try to see whether I can splice a higher order integrator into our current code without changing more than a few dozen lines.

Alice: A few dozen? That still sounds like a lot, depending how large "a few" is in your dictionary. You're so good at compressing things into a few lines. What if I challenge you: can you introduce a second-order integrator, while adding or changing no more than only a dozen lines?

Bob: You are either joking or you have an unreasonably high opinion of my programming skills. I don't want to promise anything, since I think one dozen lines is plainly unrealistic.

Alice: I was joking. Clarity over brevity, definitely. But seeing how you were glowing over brevity, I just couldn't help myself.

Bob: But perhaps I can stay under two dozen.

Alice: I shouldn't have said anything. Anyway, we'll see tomorrow!
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