Stable Circular Orbits in Planetary Motion: A Homework Solution

In summary: This is the definition of the orbit being stationary. It means that an orbit close to circular will not go too far away from being circular (the effective total energy must be larger than the effective potential).
  • #1
Prashant123
3
0

Homework Statement


Consider a particle moving in the potential U (r)= -A/r^n, where A>0. What are the values of n which admit stable circular orbits?

Homework Equations

The Attempt at a Solution


I tried to solve by putting dr/dt=0 in the total energy equation E= T + Ueff. But it didn't work. Then I came across a solution which said that for the orbit to be circular, Ueff(r) needs to have a minima when plotted against r, where Ueff is the effective potential (L^2/2mr^2+ U (r)). But I don't understand why it has to, because when n=1, where circular orbits are possible, Ueff does not have a minima since it varies with 1/r.
 
Physics news on Phys.org
  • #2
Prashant123 said:
Ueff does not have a minima since it varies with 1/r.
Yes it does. Ueff is the effective potential, not the actual potential. The effective potential includes the L^2/2mr^2 term in addition to the potential itself.
 
  • #3
Orodruin said:
Yes it does. Ueff is the effective potential, not the actual potential. The effective potential includes the L^2/2mr^2 term in addition to the potential itself.
Yes. But I want to know if the statement "circular motion is possible in this case when Ueff has a minima when plotted against r" is true and how, as for n=1, Ueff= -Gm1m2/2r and this does not have a minima.
 
  • #4
Prashant123 said:
I want to know if the statement "circular motion is possible in this case when Ueff has a minima when plotted against r" is true
It is true.

Prashant123 said:
and how, as for n=1, Ueff= -Gm1m2/2r and this does not have a minima.
You are wrong. For n=1 the potential is ##U(r) = -Gm_1m_2/r##, but the effective potential is ##U_{\rm eff}(r) = L^2/(2mr^2) + U(r) = L^2/(2mr^2) - G m_1 m_2/r##.
 
  • #5
Oh ok.. but is there a proof for why should Ueff have a minima?
 
  • #6
Prashant123 said:
Oh ok.. but is there a proof for why should Ueff have a minima?
This is the definition of the orbit being stationary. It means that an orbit close to circular will not go too far away from being circular (the effective total energy must be larger than the effective potential).
 

1. What does "stable circular orbit" mean in planetary motion?

In planetary motion, a stable circular orbit refers to the path of a planet around a central body (such as a star) that remains constant and does not deviate from its circular shape. This means that the planet's speed and distance from the central body remain constant, and the gravitational force between the two objects is balanced.

2. How is a stable circular orbit different from an elliptical orbit?

An elliptical orbit is a non-circular path, where the distance between the planet and the central body varies throughout the orbit. In contrast, a stable circular orbit has a constant distance from the central body, resulting in a circular shape. Additionally, the speed of a planet in an elliptical orbit varies, while in a stable circular orbit, the speed remains constant.

3. What factors determine the stability of a circular orbit?

The stability of a circular orbit is determined by the balance between the gravitational force of the central body and the centrifugal force of the orbiting object. The mass and distance of the central body, as well as the speed of the orbiting object, all play a role in determining the stability of the orbit.

4. Can a planet have multiple stable circular orbits around a central body?

Yes, a planet can have multiple stable circular orbits around a central body. This is known as a multi-planetary system, where planets have different stable orbits depending on their distance and speed. Our solar system is an example of a multi-planetary system, with planets like Earth and Mars having their own stable circular orbits around the Sun.

5. How do we calculate the speed and distance of a planet in a stable circular orbit?

The speed of a planet in a stable circular orbit can be calculated using the formula v = √(GM/r), where G is the gravitational constant, M is the mass of the central body, and r is the distance between the two objects. The distance of the orbit can then be calculated using the formula v²r = GM, which can be rearranged to r = GM/v².

Similar threads

  • Introductory Physics Homework Help
Replies
4
Views
2K
  • Introductory Physics Homework Help
Replies
1
Views
1K
  • Introductory Physics Homework Help
Replies
5
Views
1K
  • Introductory Physics Homework Help
Replies
18
Views
245
  • Introductory Physics Homework Help
Replies
3
Views
1K
  • Introductory Physics Homework Help
Replies
2
Views
2K
  • Introductory Physics Homework Help
Replies
1
Views
807
  • Introductory Physics Homework Help
Replies
11
Views
1K
  • Introductory Physics Homework Help
Replies
2
Views
1K
  • Introductory Physics Homework Help
Replies
4
Views
3K
Back
Top