Circular restricted three body problem

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SUMMARY

The discussion focuses on the Circular Restricted Three Body Problem, specifically investigating halo orbits and Lagrange equilibrium points. The user employs the equations of motion, particularly the second-order differential equations, to analyze particle behavior in the Earth-Sun system. They express concerns about the validity of their approach when determining the positions of orbits crossing the x-axis and the implications of y-velocity on calculations. Additionally, the conversation clarifies that numerical integration in n-body problems refers to computational methods for solving differential equations rather than traditional integral solving.

PREREQUISITES
  • Understanding of the Circular Restricted Three Body Problem
  • Familiarity with Lagrange equilibrium points
  • Knowledge of differential equations and their applications in celestial mechanics
  • Experience with numerical integration techniques for solving differential equations
NEXT STEPS
  • Explore the mathematical foundations of halo orbits in celestial mechanics
  • Learn about numerical integration methods such as Runge-Kutta for n-body simulations
  • Investigate the implications of Lagrange points in multi-body systems
  • Study the application of differential equations in modeling orbital dynamics
USEFUL FOR

Astronomers, physicists, mathematicians, and students interested in celestial mechanics and orbital dynamics will benefit from this discussion.

Deadstar
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Hey folks and happy new year!

I've been learning about the 3 body problem for a wee while now and also lagrange equilibrium points and it has got me experimenting with the same set up. I'm now investigating halo orbits and while I know you don't calculate them using this kind of method, it has given me some ideas to try out. What I've been looking at is particles crossing the x-axis perpendicular to it (as it 'appears' in pictures of halo oribts, which is where I got the idea).

Now for lagrange points, I use the (perhaps standard?) method of solving the equations of motion...

[tex]\ddot{x} - 2 \.{y} = \frac{\partial U}{\partial x}[/tex]

[tex]\ddot{y} + 2 \.{x} = \frac{\partial U}{\partial y}[/tex] (#)

Where [tex]U = \mu_1 (\frac{1}{r_1} + \frac{r_1^2}{2}) + \mu_2 (\frac{1}{r_2} + \frac{r_2^2}{2}) - \frac{1}{2}\mu_1 \mu_2[/tex] with n=1.

Setting [tex]\.{x} = \.{y} = \ddot{x} = \ddot{y} = 0[/tex].

So, now dealing with the orbits crossing the x-axis for the Earth sun 3 body system... Can I just use a method similar to the above to find the positions of these orbits on the x-axis given a y velocity..?

Does it even make sense to solve this since could we not have a particle going a certain speed at almost any point on the x-axis..?

I've been playing around and not really knowing what I've been doing but... Given that I want the particle to cross the x-axis, y will be zero and in (#), we will have to have the RHS equal to zero and hence [tex]\ddot{y} = -2 \.{x}[/tex] which seems a weird thing to presume especially given that I would have had the x velocity equal to zero but the y accel non zero! So then it's just a case of finding an expression for (in my calcs, r1) in terms of x acceleration and y velocity.

Now, if you've understood what I've been rambling about, does what I'm doing even make any sense? I can't help but feel everything is riddled with mistakes but as a mathematician I tend to not consider if what I'm doing makes physical sense and just look at what the numbers tell me...

One more quick thing to ask... I always read about people performing numerical integrations on computers for n-body problems but does this mean actually solving an integral or is it just an expression for performing numerical calculations..?
 
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Deadstar said:
One more quick thing to ask... I always read about people performing numerical integrations on computers for n-body problems but does this mean actually solving an integral or is it just an expression for performing numerical calculations..?

It's performing numerical calculations to 'follow' the trajectory (in the mathematical sense) of a system of differential equations, thus producing a numerical solution for the system. In the case of celestial mechanics, it can produce position, velocity, acceleration versus time numbers all along the trajectory (or just the 'final' position, etc., for a specified time).

Differential equations are 'integrated' to find their solution. Hence numerical integration.
 

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