  In this paper, we develop a new class of models for a compact star with
anisotropic stresses inside the matter distribution. By assuming a linear
equation of state for the anisotropic matter composition of the star we solve
the Einstein field equations. In our approach, for the interior solutions we
use a particular form of the ansatz for the metric function $g_{rr}$. The
exterior solution is assumed as Schwarzschild metric and is joined with the
interior metric obtained across the boundary of the star. These matching of the
metrices along with the condition of the vanishing radial pressure at the
boundary lead us to determine the model parameters. The physical acceptability
of the solutions has verified by making use of the current estimated data
available from the pulsar 4U1608-52. Thereafter, assuming anisotropy due to
tidal effects we calculate the Love numbers from our model and compare the
results with the observed compact stars, viz. KS 1731- 260,4U 1608- 52,4U 1724-
207,4U 1820- 30,SAX J1748.9-2021 and EXO 1745-268. The overall situation
confirms physical viability of the proposed approach,which can shed new light
on the interior of the compact relativistic objects.
