Kepler's laws of planetary motion - Revision history

FredericBernard: Added equation for Kepler's third law and some stuff about angular momentum conservation for the second

2017-04-17T16:59:58Z

Added equation for Kepler's third law and some stuff about angular momentum conservation for the second

JoeyJ at 14:20, March 10, 2016

2016-03-10T14:20:17Z

HelpJazz: Undo revision 346397 by Special:Contributions/BillOhannity (User talk:BillOhannity) no indication of copyright...?

2007-12-07T18:54:24Z

Undo revision 346397 by Special:Contributions/BillOhannity (User talk:BillOhannity) no indication of copyright...?

BillOhannity: removing copyrighted material

2007-12-03T04:12:39Z

removing copyrighted material

BillOhannity at 03:28, October 14, 2007

2007-10-14T03:28:37Z

BillOhannity: create new article Kepler's laws of planetary motion

2007-10-14T03:28:21Z

create new article Kepler's laws of planetary motion

New page

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:
1. Planets orbit the sun on [[ellipse|elliptical]] orbits with the sun occupying one of the foci of the ellipse.

2. A line connecting the sun to the orbiting body sweeps out an equal area in an equal amount of time regardless of position in the orbit. In other words, the body moves faster when it is closer to the sun and moves slower when it is further away. This law was much later shown to be true because of conservation of [[angular momentum]].

3. The square of the period of the orbit of a body is proportional to the cube of the semimajor axis of that orbit.

[[Category:Astronomy]]

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-[[File:Kepler laws diagram.png|thumb|Illustration of Kepler's three laws<br/>(1) The orbits are ellipses, with focal points ''&fnof;''<sub>1</sub> and ''&fnof;''<sub>2</sub> for the first planet and ''&fnof;''<sub>1</sub> and ''&fnof;''<sub>3</sub> for the second planet. The Sun is placed in focal point ''&fnof;''<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>&nbsp;:&nbsp;''a''<sub>2</sub><sup>3/2</sup>.]]
+[[File:Kepler laws diagram.png|thumb|Illustration of Kepler's three laws<br/>(1) The orbits are ellipses, with focal points ''&fnof;''<sub>1</sub> and ''&fnof;''<sub>2</sub> for the first planet and ''&fnof;''<sub>1</sub> and ''&fnof;''<sub>3</sub> for the second planet. The Sun is placed in focal point ''&fnof;''<sub>1</sub>. <br><br> (2) The two shaded sectors ''A''<sub>1</sub> and ''A''<sub>2</sub> have the same 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>&nbsp;:&nbsp;''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.
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 .  A line connecting the sun to the orbiting body sweeps out an equal area in an equal amount of time regardless of position in the orbit.  In other words, the body moves faster when it is closer to the sun and moves slower when it is further away.  This law was much later shown to be true because of conservation of [[angular momentum]].
-.  The square of the period of the orbit of a body is proportional to the cube of the semimajor axis of that orbit.
+.  The square of the period of the orbit of a body is proportional to the cube of the [[semi-major axis]] (the line from one side of the ellipse to the other that passes through both foci) of that orbit.
 [[Category:Astronomy]]

← Older revision		Revision as of 14:20, March 10, 2016
Line 1:		Line 1:
−	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 ''&fnof;''<sub>1</sub> and ''&fnof;''<sub>2</sub> for the first planet and ''&fnof;''<sub>1</sub> and ''&fnof;''<sub>3</sub> for the second planet. The Sun is placed in focal point ''&fnof;''<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 />

← Older revision		Revision as of 04:12, December 3, 2007
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−	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 />~~
−	~~1. Planets orbit the sun on [[ellipse\|elliptical]] orbits with the sun occupying one of the foci of the ellipse.~~
−
−	2. A line connecting the sun to the orbiting body sweeps out an equal area in an equal amount of time regardless of position in the orbit. In other words, the body moves faster when it is closer to the sun and moves slower when it is further away. This law was much later shown to be true because of conservation of [[angular momentum]].
−
−	~~3. The square of the period of the orbit of a body is proportional to the cube of the semimajor axis of that orbit.~~
−
−	~~[[Category:Astronomy]]~~

← Older revision	Revision as of 18:54, December 7, 2007
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	+	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 />
	+	1. Planets orbit the sun on [[ellipse\|elliptical]] orbits with the sun occupying one of the foci of the ellipse.
	+
	+	2. A line connecting the sun to the orbiting body sweeps out an equal area in an equal amount of time regardless of position in the orbit. In other words, the body moves faster when it is closer to the sun and moves slower when it is further away. This law was much later shown to be true because of conservation of [[angular momentum]].
	+
	+	3. The square of the period of the orbit of a body is proportional to the cube of the semimajor axis of that orbit.
	+
	+	[[Category:Astronomy]]

@@ Line 1: / Line 1: @@
 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:
+Kepler's three laws of planetary motion are:<br />
 .  Planets orbit the sun on [[ellipse|elliptical]] orbits with the sun occupying one of the foci of the ellipse.