In this paper, we introduce a framework to study the tidal deformation of relativistic 1 anisotropic compact stars. Anisotropic stresses are ubiquitous in nature and widely used in 2 modelling compact stellar object. Tidal deformability of astrophysical compact objects is a natural 3 effect of gravity such as one produced by a companion in a binary system. In general relativity, the 4 existence of this measurable effect of gravity can be quantified by their tidal Love numbers (TLN) 5 which characterize the deformability of a neutron star (NS) from sphericity. The tidal deformability 6 or polarizability parameter of a NS depends on its complex internal structure and hence the nature 7 of the compact object can study through measuring the TLN. We choose a particular solution which 8 is the anisotropic generalization of Tolman IV model as the interior of the compact stellar object. 9The physical acceptability of the model has been shown graphically by considering the pulsar 10 4U 1608-52 with their current estimated mass and radius. By computing quadrupole moment we 11 found out the TLN as a dependent on anisotropy of the compact object. We graphically analyze 12 the variation of the TLN against anisotropy for different compact objects with compactness factor. 13The numerical value of TLN is given for different compact objects for physically acceptable value 14 of anisotropic parameter.

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