How to Derive Equations of Motion for Colliding Masses in a Central Field?

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Homework Help Overview

The discussion revolves around deriving equations of motion for two colliding masses in a central gravitational field, specifically using Newton's law of gravitation. The original poster is focused on finding the time-dependent positions of the masses, r_1(t) and r_2(t), while excluding rotational motion.

Discussion Character

  • Exploratory, Assumption checking, Problem interpretation

Approaches and Questions Raised

  • The original poster attempts to integrate a derived equation involving gravitational potential energy but encounters difficulties in inverting the resulting expression for time. They also consider solving a second-order differential equation directly but feel they are missing a simple insight. Some participants question whether the signs of constants in the equations have been properly accounted for.

Discussion Status

The discussion is ongoing, with participants exploring different approaches to the problem. There is acknowledgment of the complexity involved in obtaining a closed-form solution for r(t), and some guidance has been offered regarding the integration process.

Contextual Notes

The original poster specifies that they do not wish to use Lagrangian or Hamiltonian dynamics, which may limit the methods discussed. Additionally, there is a mention of the challenge in dealing with negative constants in the equations.

PhysStudent81
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Homework Statement



I have two masses of finite width, m_1 and m_2. The force is Newton's gravity, so U = k/r. I want to work out their relevant equations of motions r_1(t) and r_2(t) as they start off from rest and collide. I don't want to consider any rotational motion.


Homework Equations



[itex]U = \frac{k}{r}[/itex]
[itex]r = r_{1}(t) - r_{2}(t)[/itex]

0.5μ[itex]\dot{r}^2 = E_{tot} - \frac{k}{r}[/itex]

dt = [itex]\frac{μ}{2}[/itex]∫[itex]\frac{dr}{\sqrt{E_{tot} - \frac{k}{r}}}[/itex]

The Attempt at a Solution



I try to integrate the above equation it gives me something very complicated (I end up integrating cosec^3 after making the substitution [itex]\frac{1}{r} = \sin^{2}(\theta)[/itex]) which gives me t = t(r), but I can't invert this to give me r = r(t).

Am I doing something wrong? Is there another way of doing it that doesn't involve lagrangian or hamiltonian dynamics (which I haven't studied).

Another way would be to solve the the 2nd order differential equation directly:

[itex]\frac{dr^{2}}{dt^{2}} = \frac{k}{r^{2}}[/itex]

but I can't seem to do this (I fee I'm missing something very simple here). I know that if I let [itex]r = At^{\frac{2}{3}}[/itex] this is a solution but it doesn't have enough constants.

Any pointers?

Thanks,

Rob
 
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PhysStudent81 said:
I try to integrate the above equation it gives me something very complicated (I end up integrating cosec^3 after making the substitution [itex]\frac{1}{r} = \sin^{2}(\theta)[/itex]) which gives me t = t(r), but I can't invert this to give me r = r(t).

Am I doing something wrong?

I think what you are doing is correct. Did you allow for the fact that both k and Etot are negative numbers? Anyway, as you say, you can get an expression for t(r). I agree that the result looks too complicated to invert for r(t).
 
So strange that for such seemingly simple problem there is no closed form result for r(t). t(r) is actually all I wanted so that's ok!
 

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