Kepler problem: flows generated by constants of motion

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SUMMARY

The discussion centers on the Hamiltonian of the Kepler problem, defined as H(𝑟,𝑝) = |𝑝²|/(2μ) + α/|𝑟|, where μ > 0 and α < 0. It establishes that the quantities 𝑚 = 𝑟 × 𝑝 and 𝑊 = 𝑝 × 𝑚 + μα(𝑟/|𝑟|) are constants of motion. The main inquiry is how to prove that the flows generated by these constants, m_i and W_i, are canonical transformations and whether they qualify as point transformations. The proof involves demonstrating that the time derivative of the transformation matches the Poisson bracket of the Hamiltonian and the transformation itself.

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Clausius
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Consider the Hamiltonian of Kepler problem
[tex]H(\boldsymbol{r},\boldsymbol{p})= \frac{|\boldsymbol{p}^2|}{2\mu} +\frac{\alpha}{|\boldsymbol{r}|}, \qquad \mu>0>\alpha,[/tex]

where [tex]\boldsymbol{r}\in M=\mathbb{R}^3\setminus\{ 0 \}, \ (\boldsymbol{r},\boldsymbol{p})\in T^*M[/tex]
and
[tex]|\boldsymbol{r}|=\sqrt{r_1^2+r_2^2+r_3^2}.[/tex]

The quantities
[tex]\boldsymbol{m}=\boldsymbol{r}\times\boldsymbol{p}, \qquad \boldsymbol{W}=\boldsymbol{p}\times\boldsymbol{m}+ \mu\alpha\frac{\boldsymbol{r}}{|\boldsymbol{r}|}[/tex]

are constants of motion, as is well known.

My question is: how can I prove that the flows generated by the functions m_i and W_i, i=1,2,3 are canonical transformations?
Moreover, are such transformations point transformations?

A canonical transformation [tex]\Phi: T^*M\to T^*M[/tex]
is a point transformation if it is induced by a transformation [tex]\phi:M\to M,[/tex]

so that
[tex]\Phi(\boldsymbol{r},\boldsymbol{p})= (\phi(\boldsymbol{r}),\phi^{*-1}), \ \phi^*_i= \frac{\partial\phi_i}{\partial r_j}p_j.[/tex]
 
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In this case, the flows generated by m_i and W_i are given by\boldsymbol{r}(t)= \boldsymbol{r}_0 + t\boldsymbol{m} \qquad \boldsymbol{p}(t)= \boldsymbol{p}_0 + t\boldsymbol{W}.To prove that these flows generate a canonical transformation, we need to show that\frac{d}{dt}\Phi(\boldsymbol{r},\boldsymbol{p})= \{H,\Phi\}.Letting \Phi(\boldsymbol{r},\boldsymbol{p})=(\boldsymbol{r}(t),\boldsymbol{p}(t)), we have\frac{d}{dt}\Phi(\boldsymbol{r},\boldsymbol{p})= (\dot{\boldsymbol{r}}(t),\dot{\boldsymbol{p}}(t)) = (\boldsymbol{m},\boldsymbol{W}).On the other hand, the Poisson bracket is given by\{H,\Phi\}= \frac{\partial H}{\partial r_i}\frac{\partial \Phi_j}{\partial p_i} - \frac{\partial H}{\partial p_i}\frac{\partial \Phi_j}{\partial r_i}.For the Hamiltonian of the Kepler problem, we have\frac{\partial H}{\partial r_i}= -\frac{\alpha r_i}{|\boldsymbol{r}|^3}, \qquad \frac{\partial H}{\partial p_i}= \frac{p_i}{\mu}.Substituting these expressions into the Poisson bracket and using the fact that \Phi(\boldsymbol{r},\boldsymbol{p})=(\boldsymbol{r}(t),\boldsymbol{p}(t)), we obtain\{H,\Phi\}= -\frac{\alpha}{|\boldsymbol{r}|^3}\left(\boldsymbol{r}\cdot\boldsymbol{m}\
 

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