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The equation T^2/R^3 (where T is the orbital period of a planet and R is its distance from the sun) is derived from Newton's Law of Universal Gravitation. By equating this equation to the known value of the gravitational constant and the mass of the sun, we can solve for the mass of the sun.
Knowing the mass of the sun is essential in understanding the dynamics of our solar system and the interactions between planets. It also helps in understanding the formation and evolution of the sun and other stars.
The calculated mass of the sun using the T^2/R^3 equation is considered to be very accurate. It has been verified by multiple experiments and is consistent with other methods of determining the mass of the sun.
Yes, the T^2/R^3 equation can be applied to any celestial body that has a known orbital period and distance from a central mass. However, the equation may need to be modified depending on the specific scenario.
One limitation is that the equation assumes a circular orbit, which is not always the case for planets. Also, the equation does not take into account the mass of the orbiting body, which may have a small effect on the calculated mass of the sun.