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The Kepler Third Law Calculator will calculate:

- The period of rotation of a celestial body around the centre of curvature (a planet for natural satellites and the Sun for planets)
- The maximum distance of a celestial body from its centre of rotation

What would you like to calculate? | |
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The period of rotation of a celestial body around the centre of curvature is s |

The maximum distance of a celestial body from its centre of rotation is m |

Period of rotation of a celestial body around the centre of curvature calculation |
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T = √ × a4 × π^{2}/(G × M)^{3}T = √ × (4 × ()^{2}/ × )^{3}T = √ × 4 × /T = √ × /T = √ × T = √ T = |

Maximum distance of a celestial body from its centre of rotation calculation |

a = ^{3}√G × M × T^{2}/4 × π^{2}a = ^{3}√ × × ^{2}/4 × ^{2}a = ^{3}√ × × /4 × a = ^{3}√/a = ^{3}√a = ( )^{1/3}a = |

Kepler Third Law Calculator Input Values |

Maximum distance of the celestial body from the centre of rotation (a) m |

Period of rotation (T) s |

The circular constant pi (π) |

Gravitational Constant (G) N∙m^{2}/kg^{2} |

Mass of the celestial body, which is at centre of rotation (M) kg |

Please note that the formula for each calculation along with detailed calculations are available below. As you enter the specific factors of each kepler third law calculation, the Kepler Third Law Calculator will automatically calculate the results and update the Physics formula elements with each element of the kepler third law calculation. You can then email or print this kepler third law calculation as required for later use.

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Calculating the period of rotation of a celestial body around the centre of curvature.

T = √*4 × π*^{2}*/**(G × M)* × a^{3}

a = ^{3}√*G × M × T*^{2}*/**4 × π*^{2}

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