„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''<sub>1</sub>. 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''<sub>Jupiter</sub> = 0.0484, just fails to qualify: 1.05 '''≯''' 1.07 > 0.954.
 
=== Animations ===
 
Images are representative, not simulated.
 
[[Fájl:orbit1.gif|bélyegkép|balra|200px|Two bodies of similar mass orbiting around a common barycenter.]]
[[Fájl:orbit2.gif|bélyegkép|200px|Two bodies with a difference in mass orbiting around a common barycenter, as in the [[Pluto]]-[[Charon (moon)|Charon]] system.]]
[[Fájl:orbit3.gif|bélyegkép|balra|200px|Two bodies with a major difference in mass orbiting around a common barycenter (similar to the [[Earth]]-[[Moon]] system)]]
[[Fájl:orbit4.gif|bélyegkép|jobbra|200px|Two bodies with an extreme difference in mass orbiting around a common barycenter (similar to the [[Sun]]-[[Earth]] system)]]
[[Fájl:orbit5.gif|bélyegkép|balra|400px|Two bodies with similar mass orbiting around a common barycenter with [[elliptic orbit]]s (a common situation for [[binary star]]s)]]
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