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| − | ==Definition==
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| − | Any orbit in planetary dynamics can be assumed to be of conic cross-section shape. The '''eccentricity''' of this conic section, the orbit's eccentricity, is an important parameter of the orbit that defines its absolute shape. Eccentricity may be interpreted as a measure of how much this shape deviates from a circle.
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| − | Eccentricity (<math>e\,\!</math>) is strictly defined for all circular, elliptic, parabolic and hyperbolic orbits and may take following values:<ref>[http://en.wikipedia.org/w/index.php?title=Orbital_eccentricity Wikipedia article on eccentricity.]</ref>
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| − | *for circular orbits: <math>e=0\,\!</math>,
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| − | *for elliptic orbits: <math>0<e<1\,\!</math>,
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| − | *for parabolic orbits: <math>e=1\,\!</math>,
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| − | *for hyperbolic orbits: <math>e>1\,\!</math>.
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| | ==Calculation== | | ==Calculation== |
Revision as of 00:54, 3 November 2011
For the love of God, keep wtrinig these articles.
Calculation
For elliptic orbits, eccentricity can be calculated from distance at periapsis and apoapsis:
where:
is distance at periapsis (closest approach),
is distance at apoapsis (farthest approach).
References
