Difference between revisions of "Eccentricity"

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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.
 
 
 
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>
 
 
 
*for circular orbits: <math>e=0\,\!</math>,
 
*for elliptic orbits: <math>0<e<1\,\!</math>,
 
*for parabolic orbits: <math>e=1\,\!</math>,
 
*for hyperbolic orbits: <math>e>1\,\!</math>.
 
  
 
==Calculation==
 
==Calculation==

Revision as of 01:54, 3 November 2011


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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