Abstract. Linear density perturbation equation for general relativistic cosmologies using the homogeneous isotropic Robertson-Walker metric and the anisotropic Bianchi-I metric for the unperturbed model has been derived in a simple and rather general manner. The method has then been applied to consideration of the fate of density perturbation in the Brans-Dicke model of the universe. Two coupled differential equations connecting variations in the density rho and the scalar field phi of the model have been obtained. An approximate solution has been sought and a power law growth of the fluctuation density, delta rho , with time has been obtained.

Print publication: Issue 2 (February 1977)