Two body problem in presence of cosmological constant
Abstract
We consider the Kepler two-body problem in presence of the cosmological constant . Contrary to the classical case, where finite solutions exist for any angular momentum of the system L, in presence of finite solutions exist only in the interval 0<L< Llim(). The qualitative picture of the two-body motion is described, and critical parameters of the problem are found. Application are made to the relative motion of the Local Group and Virgo cluster.
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