Kepler's 1st law: Difference between revisions

Latest revision as of 17:38, 1 November 2020

Johannes Kepler (b. 1571)

Kepler's laws of planetary motion 1609-1619

The orbit of every planet is an ellipse with the Sun at one of the two foci.

@@ Line 2: / Line 2: @@
 [[File:Kepler1stlaw.png|center|class=shadow|300px]]
 </div>
+'''Johannes Kepler''' (b. 1571)
+''''' Kepler's laws of planetary motion''''' 1609-1619
 The orbit of every planet is an ellipse with the Sun at one of the two foci.
-Mathematically, an ellipse can be represented by the formula:
-$${e r={\frac {p}{1+\varepsilon \,\cos \theta }},}{\displaystyle r={\frac {p}{1+\varepsilon \,\cos \theta }},}$$
-where $$p$$ is the semi-latus rectum, ε is the eccentricity of the ellipse, r is the distance from the Sun to the planet, and θ is the angle to the planet's current position from its closest approach, as seen from the Sun. So (r, θ) are polar coordinates.
-For an ellipse 0 < ε < 1 ; in the limiting case ε = 0, the orbit is a circle with the Sun at the centre (i.e. where there is zero eccentricity).
@@ Line 18: / Line 13: @@
 *[https://en.wikipedia.org/wiki/Kepler%27s_laws_of_planetary_motion#First_law_of_Kepler Kepler's 1st law]
 == Discussion: ==
+[[Category:Pages for Merging]]