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Kepler's Third Law Tutorial

Kepler's Third Law Tutorial

Kepler's Third Law:

Kepler's Third Law states that the squares of the orbital periods of planets are directly proportional to the cubes of the semi-major axis of the orbits.

Planetary Motion Formula:

Satellite Orbit Period:
Satellite Mean Orbital Radius:
Planet Mass:
where,
G = Universal Gravitational Constant = 6.6726 x 10-11N-m2/kg2 r = Satellite Mean Orbital Radius M = Planet Mass

Kepler's Third Law Examples:

Case 1: The period of the Moon is approximately 27.2 days (2.35x106 s). Determine the radius of the Moon's orbit. Mass of the earth = 5.98x1024 kg, T = 2.35x106 s, G = 6.6726 x 10-11N-m2/kg2.

Step 1:

Substitute the values in the below Satellite Mean Orbital Radius equation:

This example will guide you to calculate the Satellite Mean Orbital Radius manually. Case 2: Determine lo's mass, which orbits Jupiter at an orbital radius of 4.218 x 108 at every 151200 seconds. r = 4.218 x 108 m, T = 151200 s, G = 6.6726 x 10-11N-m2/kg2.

Step 1:

Substitute the values in the below Mass equation:

This example will guide you to calculate the Mass of the object manually.


This tutorial will help you dynamically to find the Planetary Motion of Kepler's Third Law problems.

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