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The equation is M = (v^2 * r) / G, where M is the mass of the sun, v is the orbital speed of a planet, r is the distance between the planet and the sun, and G is the gravitational constant.
This method is highly accurate, with an error margin of less than 0.1%. It is widely used by astronomers and scientists to estimate the mass of celestial bodies.
The value of G is approximately 6.674 x 10^-11 m^3/kg*s^2. This is a universal constant that represents the strength of gravitational force between two objects with mass.
Yes, this equation can be used to estimate the mass of any celestial body as long as the distance and speed of a planet orbiting around it are known.
This method was developed using Newton's laws of motion and universal gravitation. It was first used by scientists and astronomers in the 18th century to accurately calculate the mass of the sun.