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Abstract
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In the framework of f(R) scalar-tensor cosmology, we use the Noether symmetry approach
to fi nd the cosmological models consistent with the Noether symmetry. We obtain the
functions f(R) and H(a), or the corresponding di erential equations, according to speci c
choices for the scalar eld potential V (phi ), the Brans-Dicke function w(phi ), some cosmological
parameters, and the constants of motion. This enables us to choose the viable scalar-tensor
cosmologies from the Noether symmetry point of view.
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