Orbital eccentricity - Revision history

Lilly Schoen at 12:01, 2 November 2017

2017-11-02T12:01:43Z

Lilly Schoen at 12:01, 2 November 2017

2017-11-02T12:01:25Z

Lilly Schoen: Created page with "{{GlossaryTermTemp |SubtermOf=eccentricity |Definition=1. The orbital eccentricity of an astronomical object is a parameter that determines the amount by which its orbit arou..."

2017-11-02T12:00:20Z

Created page with "{{GlossaryTermTemp |SubtermOf=eccentricity |Definition=1. The orbital eccentricity of an astronomical object is a parameter that determines the amount by which its orbit arou..."

New page

{{GlossaryTermTemp
|SubtermOf=eccentricity
|Definition=1. The orbital eccentricity of an astronomical object is a parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptical orbit, 1 is a parabolic escape orbit, and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a rosette orbit through the galaxy.
2. The orbital eccentricity refers how elliptical earth’s orbital path is. The greater the eccentricity of a planet’s orbital path, the less circle-like and more elliptical (oval-like) it is. An ellipse has an eccentricity greater than or equal to zero, but less than one. An eccentricity value of e = 0 corresponds to a perfect circle, whereas e = 1 corresponds to a parabola, and e > 1 corresponds to a hyperbola. At higher eccentricity values (albeit less than one), there is a greater discrepancy between a planet’s perihelion and aphelion: a planet’s nearest and furthest points from the sun during its orbit.
|Sources=https://en.wikipedia.org/wiki/Orbital_eccentricity (1.); http://www.wikiwand.com/en/Real-time_data (2.)
}}
Author: Thomas D.

@@ Line 5: / Line 5: @@
 |Sources=https://en.wikipedia.org/wiki/Orbital_eccentricity (1.); http://www.wikiwand.com/en/Real-time_data (2.)
 }}
-Author: <span>Simon</span><span class="b"></span><span>Waterstradt</span>
+Author: <span>Simon </span><span class="b"></span><span>Waterstradt</span>

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 {{GlossaryTermTemp
 |SubtermOf=eccentricity
 |Definition=1. The orbital eccentricity of an astronomical object is a parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptical orbit, 1 is a parabolic escape orbit, and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a rosette orbit through the galaxy.
 . The orbital eccentricity refers how elliptical earth’s orbital path is. The greater the eccentricity of a planet’s orbital path, the less circle-like and more elliptical (oval-like) it is. An ellipse has an eccentricity greater than or equal to zero, but less than one. An eccentricity value of e = 0 corresponds to a perfect circle, whereas e = 1 corresponds to a parabola, and e > 1 corresponds to a hyperbola. At higher eccentricity values (albeit less than one), there is a greater discrepancy between a planet’s perihelion and aphelion: a planet’s nearest and furthest points from the sun during its orbit.
 |Sources=https://en.wikipedia.org/wiki/Orbital_eccentricity (1.); http://www.wikiwand.com/en/Real-time_data (2.)
 }}
-Author: Thomas D.
+Author: <span>Simon</span><span class="b"></span><span>Waterstradt</span>