Question

The following equation, derived from Newton's version of Kepler's third law, allows us to calculate the mass (m) of a central object, in solar masses, from an orbiting object's period (p) in years and semimajor axis (a) in astronomical units: a. m = p^2 / a^3 b. m = p^3 / a^2 c. m = p / a d. m = p * a^2

Answer 1

The correct equation to calculate the mass of a central object in solar masses is m = p^2 / a^3. This equation is derived from Newton's version of Kepler's third law for binary star systems.

the correct answer is a m = p^2 / a^3

Step-by-step explanation:

Kepler's third law states that the square of the orbital period is proportional to the cube of the semimajor axis of the orbit. In the case of calculating the mass of a central object in solar masses from an orbiting object's period and semimajor axis, the correct equation is m = p^2 / a^3.

This equation is derived from Newton's version of Kepler's third law (D³ = (M₁ + M₂) P²) for binary star systems.

the correct answer is a m = p^2 / a^3