Solving a Fairly Simple Gravity Problem with Negligible Air Resistance

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In summary: and it's used to show that a particle will require about 9/11 of the time to fall half way to the ground based on the gravitational force and air resistance.
  • #1
PiratePhysicist
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I named my original post poorly, so this one is meant to just rename it, my work so far can be found in https://www.physicsforums.com/showthread.php?t=191219

1. Problem: A particle falls to Earth starting from rest at a great height (may times Earth's radius ). Neglect air resistance and show that the particle requires approximately 9/11 of the total time of fall to traverse the first half of the distance.

2. Homework Equations :
[tex]F=\frac{-G M_e m}{r^2}[/tex]

3. Attempt at the solution:
https://www.physicsforums.com/showthread.php?t=191219
 
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  • #2
PiratePhysicist said:
I named my original post poorly, so this one is meant to just rename it, my work so far can be found in https://www.physicsforums.com/showthread.php?t=191219

1. Problem: A particle falls to Earth starting from rest at a great height (may times Earth's radius ). Neglect air resistance and show that the particle requires approximately 9/11 of the total time of fall to traverse the first half of the distance.

2. Homework Equations :
[tex]F=\frac{-G M_e m}{r^2}[/tex]

3. Attempt at the solution:
https://www.physicsforums.com/showthread.php?t=191219

I think what you need to do is, at this point:

[tex]v^2=2G M_e ( \frac{1}{r}-\frac{1}{r_0})[/tex]

let r0 = infinity...

then continue from there.

although your derivation using separable diff. eq. was all correct... you can use conservation of energy to do that, unless you haven't covered energy yet...
 
  • #3
Nope, tried something similar (redefined axises so [tex]r_0[/tex] was 0), here's what happens:
[tex]\frac{dr}{dt}=\sqrt{\frac{2 G M_E}{r}}[/tex]
[tex]\sqrt{r}dr=\sqrt{2 G M_E}dt[/tex]
[tex]\frac{2}{3}r^{\frac{3}{2}}=sqrt{2G M_E}t[/tex]
[tex]t=\frac{2}{3}\sqrt{\frac{r^3}{2GM_E}}[/tex]
So if you take the ratio of t(1/2r) and t(r) you get
[tex]\frac{\frac{2}{3}\sqrt{\frac{(\frac{r}{2})^3}{2GM_E}}}{\frac{2}{3}\sqrt{\frac{r^3}{2GM_E}}}[/tex]
Which boils down to
[tex](1/2)^\frac{3}{2}[/tex] which is equal to .353535... not .8181818181
 
  • #4
PiratePhysicist said:
[tex]\frac{2}{3}r^{\frac{3}{2}}=sqrt{2G M_E}t[/tex]

Won't there be a non-zero integration constant to be evaluated?

The original differential equation

[tex]\frac{dr}{dt}=\sqrt{\frac{2 G M_E}{r}}[/tex]

describes an outbound trajectory, since the right-hand side is positive. Infall should require the insertion of a minus sign, no? In any case, dr/dt is only zero according to this equation for r -> infinity; then you have a separate can of worms in describing when you have fallen halfway from infinity. If you start from a finite distance out (or time-reverse the path, start from the Earth's surface, and look at the times when the particle reaches (r0/2) and r0, the integration is incomplete as it stands...
 
  • #5
Erm, my long drawn out derivation, was meant to show that the take to infinity assumption doesn't work, but your explanation works better and doesn't require lots of LaTeX ^_^

So anyone else have any suggestions?
 
  • #6
Something seems suspect about that 9/11 value. You can treat the "radial infall" problem using Kepler's Third Law on what are called "degenerate orbits".

Compare the fall from r0 with a fall from (r0/2) by treating each as having a pericenter at r = 0 and the apocenters at r0 and (r0/2), respectively. Then the "semi-major axes" of these degenerate ellipses are a1 = (r0/2) and a2 = (r0/4). The respective times to reach r = 0 are the half-periods of these "orbits"

T1 = (1/2)·sqrt[ {4·(pi^2)/GM} · (r0/2)^3 ] and
T2 = (1/2)·sqrt[ {4·(pi^2)/GM} · (r0/4)^3 ] ;

in other words, basically what you found by integrating the energy result (and starting from the gravitational force equation takes you to the same place).

The ratio of the infall times is T2/T1 = (1/2)^(3/2) = 0.3536... , as you already found. (This is a standard astrophysical exercise.) The time to fall the last half is 0.354 of the time to fall the full distance, so the time to fall the first half is about 0.646 of the total infall time.

That former value is very close to 4/11 = 0.363636... , which makes me wonder if there was a handwriting issue and whether the writer confused the statement of the problem. (This would make the answer to the stated question about 7/11 of the total time.) I think your derivation is basically correct; the 9/11 didn't sound right to me from the start, but I thought maybe I was recalling something incorrectly...
 
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  • #7
The 9/11 number comes from the book (Classical Dynamics of Particles and Systems 5th Ed Thornton and Marion)
 

1. What is the concept of "Fairly Simple Gravity Problem"?

The concept of "Fairly Simple Gravity Problem" refers to a type of physics problem that involves calculating the force of gravity between two objects. It is considered fairly simple because it only involves two objects and assumes no external factors or complexities.

2. How do you solve a "Fairly Simple Gravity Problem"?

To solve a "Fairly Simple Gravity Problem", you need to use the formula F = G(m1m2)/r^2, where F is the force of gravity, G is the gravitational constant, m1 and m2 are the masses of the two objects, and r is the distance between them. Plug in the values and solve for the force of gravity.

3. What are some real-life examples of "Fairly Simple Gravity Problems"?

Real-life examples of "Fairly Simple Gravity Problems" include calculating the force of gravity between two planets, two orbiting satellites, or a planet and a moon. It can also be used to calculate the gravitational force between a person and the Earth.

4. What are the limitations of using "Fairly Simple Gravity Problems"?

One limitation of using "Fairly Simple Gravity Problems" is that it assumes a perfect spherical shape for the objects and does not take into account any external factors such as air resistance or other forces acting on the objects. It also only works for point masses and cannot be used for objects with irregular shapes.

5. How does "Fairly Simple Gravity Problem" relate to other concepts in physics?

"Fairly Simple Gravity Problem" is closely related to other concepts in physics such as Newton's Law of Universal Gravitation and the concept of gravitational potential energy. It is also an important component in understanding orbits and the motion of objects in space.

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