Astronomy - Determine the sum of the stellar masses

AI Thread Summary
To determine the sum of the stellar masses for a double star system 10 light years away, the maximum angle observed between the stars is 2 arcseconds, which can be used to calculate the actual distance between them using basic trigonometry. The gravitational force must equal the centripetal force, leading to the formulation of equations that relate the masses and their orbital characteristics. The angular velocity is derived from the rotation period of 4 years, allowing for the expression of the sum of the masses as M+m=(2π/T)²(R+r)³/G. The challenge lies in calculating the distance (R+r) based on the provided angle and distance from Earth. Basic trigonometric principles will aid in this calculation.
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Homework Statement


A double star located at a distance of 10 light years from us. The maximum angle between the stars, as seen from Earth, is 2 arcseconds. (1 arcsecond = 1 / 3600 degrees), we can assume that the stellar orbit is circular and that this angle gives us the real distance between the stars. We observe that the rotation period of the stars is 4 years. What is the sum of stellar masses?

Homework Equations


Newton's law of universal gravitation:
F_{G}=G\frac{m_{1}m_{2}}{r^{2}}
Centripetal force:
F_c=\frac{mv^2}{r}
Kepler's third law:
P^{2} \propto a^{3}

The Attempt at a Solution


The stellar orbit is circular, so the gravitational force should be equal to the centripetalforce, but how do I proceed?
 
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You can work out the actual distance between the two bodies by simple geometry. You should also realize that the both bodies will orbit a common center of mass, so you can work out the individual radii of their orbits (symbolically) as fractions of that distance which depend upon their relative masses. Their individual velocities can similarly be determined (symbolically) from the resulting circumferences of their orbits and the given period of the orbit.

These, along with your gravitational force and centripetal force expressions, should allow you to find an expression for the sum of the two masses.
 
I rewrite the centripetal force as:
F_{c}=m\cdot \omega^{2}\cdot r

So now I can express the equality between the gravitational force and centripetal force for respective star to be
M\omega^{2}R=G\frac{Mm}{(R+r)^{2}}
m\omega^{2}r=G\frac{Mm}{(R+r)^{2}}

I simply the expression and then and I add the left-hand side of the equations together and the same procedure to the right-hand side and I find this expression for the sum of the masses:
M+m=\frac{\omega^{2}\cdot (R+r)^{3}}{G}

The angular velocity can be expressed as
\omega=\frac{2\pi}{T}

I finally found this expression for the sum of the masses:
M+m=\frac{(\frac{2\pi}{T})^{2}\cdot (R+r)^{3}}{G}
But I’m not sure how I’ll proceed and calculate the distance (R+r), should I relate the distance from Earth and the maximum angle between the stars?
 
tosv said:
But I’m not sure how I’ll proceed and calculate the distance (R+r), should I relate the distance from Earth and the maximum angle between the stars?

Yes. Basic trig.
 
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