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The motion of a mass in a gravitational field, deriving equations for the trajectories and energies involved. The two types of motion and their corresponding energies, as well as stable and unstable equilibria. It also provides equations for the velocity and position as functions of time.
Typology: Exercises
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s equations, q˙ = ∂H/∂p = p/mr^2 , and p˙ = −∂H/∂q = −mGr sin q. Thus, ¨q = p˙/mr^2 = −G sin q/r. (Again, factors of r require adjustment.)
5 On a given trajectory, H(q, p) takes some constant value E. Since cos q ≤ 1 , I have
p^2 = 2mr^2 (E + mGr cos q) ≤ 2 mr^2 (E + mGr),
or −r
2 m(E + mGr) ≤ p ≤ r
2 m(E + mGr).
Note that in order for this to make sense, I must have E ≥ −mGr, so energies strtictly less than −mGr are inaccessible. (This makes sense physically, since −mGr is the potential energy when the mass is at its lowest position.) Similarly, since cos q ≥ − 1 , I have p^2 ≥ 2 mr^2 (E − mGr). Thus, p = 0 will never oc- cur when E > mGr. Remembering that E < −mGr is impossible, then, there are 2 broad types of mo- tion and 2 degenerate energies. When |E| < mGr, the motion will pass through p = 0 but will never reach cos q = − 1. Physically, this corresponds to an oscillation about the bottom position. When E > mGr, in contrast, the motion will pass through cos q = − 1 but will never reach p = 0. Physically, this corresponds to traversing the entire conguration space. One degenerate energy is E = −mGr, where the motion re- mains at cos q = 1 and p = 0, a stable equilibrium. Physically, this corresponds to remaining in the bot- tom position. The other degenerate energy is E = mGr. In this case, we could have p = 0 and cos q = − 1 , another equilibrium. However, this is not required; we could have p > 0 and cos q > − 1 , or alternatively p < 0 and cos q > − 1. This trajectory would approach the above equilibrium but never reach it. There- fore, this equilibrium is unstable. Physically, the unstable equilibrium corresponds to balancing at the top position, as indicated in digression 2, and the degenerate trajectory approaching this equilibrium corre- sponds to ever more slowly climbing to the top. A graph illustrating this is on the next page.
6 As already noted, p^2 = 2mr^2 (E + mGr cos q). Since q˙ = p/mr^2 , it follows that q˙^2 = 2(E + mGr cos q)/mr^2 ,
so q˙ = ±
2(E + mGr cos q)/mr^2 , which is equation (1) with the correct factors of r.
7 Of course, we really want mGr = 1, not so much mG = 1. (Note that the product m^2 r^2 G of these units gives a scale for p^2 , as can be seen on the graph for problem 5, while the quotient G/r gives a scale for t^2 .) Then the previous problem gives q˙^2 = 2(E + cos q). Since dt = dq/˙q, equation (2) follows if I use the principal square root. Note that this will break down when p changes sign, which can happen when |E| < 1 in the new units (the oscillating case).
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8 The minimum value for the energy is − 1 in these new units, so the formula oered for the modulus k must make sense. Since x = sin (q/2)/k, I have x˙ = ˙q cos (q/2)/2k, so
x ˙^2 = ˙q^2 cos^2 (q/2)/4k^2 = (E + cos q)(1 + cos q)/4k^2 = (2k^2 − 1 + cos q)(1 + cos q)/4k^2.
Meanwhile, x^2 = (1 − cos q)/2k^2 , so 2 k^2 − 1 + cos q = 2k^2 (1 − x^2 ), and 1 + cos q = 2(1 − k^2 x^2 ). Thus, x ˙^2 = (1 − x^2 )(1 − k^2 x^2 ). Now, in the oscillating case, our analysis will already break down at cos q = −E, or 1 − x^2 = 0; in the case of perpetual rotation, on the other hand, 1 − x^2 is always strictly positive. In that case, furthermore, x˙ will remain nonnegative so long as cos (q/2) does, a simplication that breaks down at cos q = − 1 , or 1 − k^2 x^2 = 0; but in the oscillating case, that is never reached. Thus in either case, the formula x˙ =
(1 − x^2 )(1 − k^2 x^2 ) will be valid on any interval containing x = 0 where it makes sense. (The degenerate nonequilibrium will nd this formula valid and true always, while the equilibria will nd the formula never dened.) Formula (3) then follows, so long as it is applied on an interval containing 0.
9 Here I indeed integrate on an interval containing 0. The correct form may vary from that given by a con- stant, but since it gives the correct value t = 0 for x = 0, it must be exactly right. We can now dene the elliptic function sn for all values of x by making recourse to the physical problem of the pendulum, since that denition agrees with the integral whenever the latter makes sense.
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