Does Kepler's Second Law Indicate Variable Orbital Speeds?

  • Thread starter Saladsamurai
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In summary, the text states that as a planet moves closer to the Sun its speed decreases, and this can be proved using the principle of area.
  • #1
Saladsamurai
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whether a planet moves faster or slower when it is closer to the Sun.

Now I intuitively know that is [tex]\frac{dA}{dt}[/tex] is constant and the Radius r is changing. Then as r increases it moves slower and as r decreases is moves faster.

I am having trouble setting up a more formal proof.

I am thinking I will need to use the relationship [tex]L=\vec r*\vec p[/tex]

Please send a hint my way.

Thanks,
Casey
 
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  • #2
Use right triangles to approximate the area swept...
 
  • #3
[tex]T = 2\pi \sqrt {\frac{r}{glocal}}[/tex]

This is a great formula that'll solve a lot of questions for you in times of need. Just remember that it's the same as the pendulum formula, only that g is the strength of Earth's gravitational field at the point of the satellite. This is only valid for orbits with low eccentricities.

[tex]g[/tex]local[tex] = \frac {9.8} {R^2} [/tex] where R is a number that is in terms of Earth's radius. i.e. 2 radii from Earth's CoM. You can use:

[tex]g[/tex]local [tex] = \frac{GM} { r^2}[/tex] if you don't like using shortcuts.
 
  • #4
Opps, that's Kepler's 3rd law.

The second law is about area, so yeah, use triangles.
 
  • #5
What you could do is consider two traingles of small but equal areas. One representing the distance to the nearer part and other to the farther part. The areas of these two triangles are same, and one side of each triangle represents the distance covered by the two objects in the same time.

Areas of triangles are equal,

1/2*d1*r1=1/2*d2*r2 -- where r1 and r2 are perpendiculars drawn from focus to d1,d2, which thus represent the radius approximately.

d1*r1 = d2*r2

If r1<r2, then d1>d2. Thus proved.

The above proof is a very crude proof I came up with, but still it works quite a bit.

Regards,
Sleek.
 
  • #6
learningphysics said:
Use right triangles to approximate the area swept...
The text makes reference to this method and I can sort of follow it, but I have some questions...but I first have to figure out how to word them!

So if I draw radius r from the Sun focus F to any point on the ellipse, and then a small line extending out from it at 90 degreesand then connect that line to the focus as well...I have a right triangle whose area id approximate to that of the area swept out ...I wish I could draw this in LaTex.

...to be continued shortly...
 
  • #7
Sleek said:
What you could do is consider two traingles of small but equal areas. One representing the distance to the nearer part and other to the farther part. The areas of these two triangles are same, and one side of each triangle represents the distance covered by the two objects in the same time.

Areas of triangles are equal,

1/2*d1*r1=1/2*d2*r2 -- where r1 and r2 are perpendiculars drawn from focus to d1,d2, which thus represent the radius approximately.

d1*r1 = d2*r2

If r1<r2, then d1>d2. Thus proved.

The above proof is a very crude proof I came up with, but still it works quite a bit.

Regards,
Sleek.

Sleek, I think I may be able to work something out of this, however as in my description above I think my right angle is in a different spot...however it may not matter, seeing as there is indeed a right angle and my r is indeed r.
I will upload a pic.

Now how can I write this out quantitatively to state that as r increase speed must decrease since dA/dt is constant?

Casey
 

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  • #8
In the below image, you can see two traingles, with equal areas and a perpendicular dropped to both of their "bases", which is an approximation of the distance covered by a body. I've exaggerated the size of the triangles, so the real distance and the distance represented by the base of the triangles might look distinct, but we're assuming triangles with very small areas.
http://img398.imageshack.us/img398/511/ellipseimgro7.th.jpg
What we do is, from a focus of an ellipse, we draw two lines to a longer and smaller side of the ellipse, which is indeed the radii r1 and r2. Then we construct the bases of both triangles such that its perpendicular to the radii and the areas of both triangles are equal and infinitesimally small. The digram is larger just for clarity.

By equating areas of both triangles as before, we get

since r1<r2, d1>d2.

For a specific time interval, a body travels d1 distance when nearer to focus and d2 when far away such that d1>d2. But it covers both this distance in the same time t. Thus speed nearer to the focus is larger.

I could not see your attached picture since it is still pending approval.
 
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  • #9
Saladsamurai said:
Sleek, I think I may be able to work something out of this, however as in my description above I think my right angle is in a different spot...however it may not matter, seeing as there is indeed a right angle and my r is indeed r.
I will upload a pic.

Now how can I write this out quantitatively to state that as r increase speed must decrease since dA/dt is constant?

Casey

Hint: rw = v. So dA/dt = (1/2)rv
 

1. How do I use Kepler's 2nd law to show the relationship between a planet's orbital period and its distance from the sun?

To use Kepler's 2nd law, also known as the Law of Equal Areas, you will need to know the planet's orbital period (the time it takes to complete one orbit around the sun) and its distance from the sun. Then, you can calculate the area swept out by the planet's orbit in a specific amount of time. This area will be equal regardless of the planet's distance from the sun, showing the relationship between the two.

2. What is the significance of Kepler's 2nd law in understanding planetary motion?

Kepler's 2nd law is significant because it helps us understand that a planet's speed changes as it moves around the sun. This law states that as a planet gets closer to the sun, it moves faster, and as it moves farther away, it slows down. This explains why planets have varying orbital speeds and also helps us understand how they maintain stable orbits.

3. Can Kepler's 2nd law be applied to objects other than planets?

Yes, Kepler's 2nd law can be applied to any object orbiting around another object, as long as we know the orbital period and distance from the center of mass. This law applies to satellites, comets, and even artificial objects like spacecraft.

4. How did Kepler discover his 2nd law?

Kepler discovered his 2nd law by carefully studying the observations and data of his predecessor, Tycho Brahe. He noticed that the speed of a planet's orbit changes as it moves around the sun, and through further calculations and observations, he was able to formulate the Law of Equal Areas.

5. Is Kepler's 2nd law still relevant in modern astronomy?

Yes, Kepler's 2nd law is still a fundamental principle in modern astronomy and is used to understand the motion of planets and other objects in our solar system. It has also been applied to other systems, such as binary stars, to better understand their orbital patterns.

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