„Tömegközéppont” változatai közötti eltérés

 

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The calculations above are based on the mean distance between the bodies and yield the mean value ''r''₁. But all celestial orbits are eliptical, and the distance between the bodies varies between the [[apsis|apses]], depending on the [[eccentricity (orbit)|eccentricity]], ''e''. Hence, the position of the barycenter varies too, and it is possible in some systems for the barycenter to be ''sometimes inside and sometimes outside'' the more massive body. This occurs where:

 

 

Note that the Sun-Jupiter system, with ''e''_Jupiter = 0.0484, just fails to qualify: 1.05 '''≯''' 1.07 > 0.954.

 

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