Posted by Me on Wednesday, November 30, 2011 at 10:49pm.
I have answered it once and will not do it again.
http://www.jiskha.com/display.cgi?id=1322287372
Yes, thank you but as I said, I still can not figure out from what you gave me so maybe someone else will explain better (figuring out the mass of the star that is).
The reference I gave you for Kepler's Third Law did not solve the problem for stars other than the sun. A better reference would be
http://www.astro.cornell.edu/academics/courses/astro101/java/Finding%20Exosolar%20Planets.htm
There, you will find the formula.
P^2 = 4 pi^2*r^3/[G*(m1 + m2)]
The author also derives it there.
In your case, ignore the planet's mass m2 because it will be negligible compared to the star's mass, m1.
P is the period, 368 days = 3.18*10^7 s
r is the orbital radius, 1.59*10^11 m.
Look up the value of G and solve for the star's mass m1, in kilograms.
It should be not much different from the sun's mass, because the r and P values you are using are close to those of the Earth orbiting the sun.
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