The theory of an induced energy polarized vacuum is used to determine the rotational curves for modeled galaxies whose baryonic mass distribution parameters are the median values of three classes of spiral galaxies. From the theoretical curves it is found that the bulge contribution plays a dominant role in determining the behavior of the rotational curves in the inner regions (i.e., within three disc scale lengths). For the outer regions the theoretical rotational curves for all the galaxies behave similarly as they slowly fall to the asymptotic value as determined by the baryonic Tully-Fisher relationship. Overall it is found that rotational curves generated by the induced energy polarized vacuum theory can readily produce observed features in the rotational curves of spiral galaxies.
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