In the frame work of TREDER's gravitational theory we consider two classes of field equations which are derivable from two classes of LAGRANGEian densities Ω(1)1, ω2), Ω(2)(s̀1, s̀2). ω1, ω2; s̀1, s̀2 are parameters. Ω(2)1, ω2) gives us field equations which are up to the post-NEWTONian approximation in the sense of NORDTVEDT, THORNE and WILL equivalent to the field equations given by BRANS and DICKE. For ω2 = −1 −2ω1 field equations follow from Ω(1)1, −1 −2ω1) which are in the above mentioned sense of post-NEWTONian approximation equivalent to EINSTEIN's equations. The field equations following from Ω(1)1, ω2) have a cosmological model with the well known cosmological singularities for T [RIGHTWARDS ARROW] ± ∞ in case that ω1/(1 +3ω12) [TRIPLE BOND] γ > 0. For ω1/(1 +3ω12) ≤ 0 cosmological models with no cosmological singularities exist.

From Ω(2)(s̀1, s̀2) we obtain field equations which at the best give us perihelion rotation 7% above EINSTEIN's value and light deflection 7% below the corresponding EINSTEIN's value. But in that case we are able to show the existence of a cosmological model without any cosmological singularity.