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Kepler's laws of planetary motion (view source)
Revision as of 14:20, March 10, 2016
, 14:20, March 10, 2016no edit summary
Kepler's three laws of planetary motion were developed in the early 17th century by [[Johannes Kepler]]. Kepler developed the laws after studying the astronomical observations of [[Tycho Brahe]] for several years. Kepler realized that the movement of the celestial bodies whose data Brahe had recorded did not fit a circular orbit, as was believed at the time.
[[File:Kepler laws diagram.png|thumb|Illustration of Kepler's three laws<br/>(1) The orbits are ellipses, with focal points ''ƒ''<sub>1</sub> and ''ƒ''<sub>2</sub> for the first planet and ''ƒ''<sub>1</sub> and ''ƒ''<sub>3</sub> for the second planet. The Sun is placed in focal point ''ƒ''<sub>1</sub>. <br><br> (2) The two shaded sectors ''A''<sub>1</sub> and ''A''<sub>2</sub> have the same surface area and the time for planet 1 to cover segment ''A''<sub>1</sub> is equal to the time to cover segment ''A''<sub>2</sub>. <br><br> (3) The total orbit times for planet 1 and planet 2 have a ratio ''a''<sub>1</sub><sup>3/2</sup> : ''a''<sub>2</sub><sup>3/2</sup>.]]
'''Kepler's three laws of planetary motion''' were developed in the early 17th century by [[Johannes Kepler]]. Kepler developed the laws after studying the astronomical observations of [[Tycho Brahe]] for several years. Kepler realized that the movement of the celestial bodies whose data Brahe had recorded did not fit a circular orbit, as was believed at the time.
Kepler's three laws of planetary motion are:<br />
Kepler's three laws of planetary motion are:<br />