The Tensor-Vector-Scalar theory of gravity, which was designed as arelativistic implementation to the modified dynamics paradigm, has fared quitewell as an alternative to dark matter, on both galactic and cosmologicalscales. However, its performance in the solar system, as embodied in thepost-Newtonian formalism, has not yet been fully investigated. Tamaki hasrecently attempted to calculate the preferred frame parameters for TeVeS, butignored the cosmological value of the scalar field, thus concluding that theNewtonian potential must be static in order to be consistent with the vectorequation. We show that when the cosmological value of the scalar field is takeninto account, there is no constraint on the Newtonian potential; however, thecosmological value of the scalar field is tightly linked to the vector fieldcoupling constant K, preventing the former from evolving as predicted by itsequation of motion. We then proceed to investigate the post-Newtonian limit ofa generalized version of TeVeS, with {\AE}ther type vector action, and showthat its \beta,\gamma and \xi parameters are as in GR, while solar systemconstraints on the preferred frame parameters \alpha_1 and \alpha_2 can besatisfied within a modest range of small values of the scalar and vector fieldscoupling parameters, and for values of the cosmological scalar field consistentwith evolution within the framework of existing models.
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