How Does Binary Star Mass Calculation Using Kepler's Law Work?

Click For Summary

Homework Help Overview

The discussion revolves around calculating the mass of binary stars using Kepler's laws, specifically focusing on a scenario where two stars are in orbit around each other with a given separation and orbital period.

Discussion Character

  • Conceptual clarification, Mathematical reasoning, Assumption checking

Approaches and Questions Raised

  • Participants explore the application of Kepler's laws to derive the mass of binary stars, with some attempting to rearrange formulas and others questioning the assumptions made regarding the mass of the stars and the interpretation of distance.

Discussion Status

There are multiple interpretations of the equations used, with participants identifying potential mistakes in each other's approaches. Some guidance is offered regarding the application of Kepler's laws to binary systems, but no consensus is reached on the correct method or outcome.

Contextual Notes

Participants note the importance of understanding the assumptions behind Kepler's laws, particularly regarding the relative masses of the stars and the interpretation of the orbital radius.

lindz.12
Messages
6
Reaction score
0
Consider a pair of binary stars with a separation of 3.60E12 m and an orbital period of 2.55E9s. Assuming the two stars are equally massive, determine the mass of each.

keplar's law...
so I rearranged the formula and set (2pi*r)/T=sqrt((GM)/r), and then I solved for M, which gave me the equation M={[4(pi)^2](r^3)}/(GT^2). Then, I solved for it, and I got 5.3E29kg.


i know the distance given to me was like the diameter, so technically, the radius would be 1.8E12; also, is M the mass of one binary star, considering this question is saying a pair of binary stars...

can someone tell me what i did wrong?
 
Physics news on Phys.org
I get M={[16(pi)^2](r^3)}/(GT^2) if you use R eq. half the distance. Because, in that case, (2pi*r)/T=sqrt((GM)/2r). Because the force due to gravity is (M^2)G/4(R^2)
 
Last edited:
thank you!
 
Both of these results are wrong.

lindz.12 said:
keplar's law...
so I rearranged the formula and set (2pi*r)/T=sqrt((GM)/r), and then I solved for M, which gave me the equation M={[4(pi)^2](r^3)}/(GT^2). Then, I solved for it, and I got 5.3E29kg.

ak1948 said:
I get M={[16(pi)^2](r^3)}/(GT^2) if you use R eq. half the distance. Because, in that case, (2pi*r)/T=sqrt((GM)/2r). Because the force due to gravity is (M^2)G/4(R^2)

So, what's wrong? lindz.12, your mistake was in using Kepler's laws. These laws are an approximation that implicitly assume that the mass of the orbiting body is very small compared to the mass of the central body. ak1948, your mistake was in using an invalid equation.

Kepler's third law can be extended to cover the case of a pair of masses orbiting one another such that neither mass can be deemed to be negligibly small. In this case,

\tau^2 = \frac{4\pi^2a^3}{G(M_1+M_2)}

where a is the semi-major axis of the orbit of the bodies about each other (i.e., not about their center of mass).Edit:
Solving for the masses,

M_1+M_2 = \frac{4\pi^2a^3}{G\tau^2}
 
Last edited:
DH
I think its the same result: what you call "a" I called "2R". what you call M1+ M2 I call 2M.
 

Similar threads

  • · Replies 7 ·
Replies
7
Views
1K
  • · Replies 10 ·
Replies
10
Views
3K
Replies
10
Views
3K
  • · Replies 2 ·
Replies
2
Views
3K
  • · Replies 2 ·
Replies
2
Views
2K
  • · Replies 2 ·
Replies
2
Views
6K
  • · Replies 7 ·
Replies
7
Views
4K
Replies
5
Views
3K
  • · Replies 4 ·
Replies
4
Views
5K
  • · Replies 3 ·
Replies
3
Views
1K