  The present work discusses about the existence of compact star model in the
context of $f(R,T)$ gravity with $R$ as the Ricci scalar and $T$ as the trace
of energy-momentum tensor $T_{\mu \nu}$. The model has been developed by
considering the spherically symmetric spacetime consisting of isotropic fluid
with $f(R,T)=R+2 \beta T$ with $\beta$ be the coupling parameter. The
corresponding field equations are solved by choosing well known Finch-Skea {\em
ansatz} [Finch, M.R., Skea, J.E.F.:{\it Class. Quantum Gravity} {\bf 6}, 467
(1989)]. For spacetime continuity we elaborate the boundary conditions by
considering the exterior region as Schwarzschild metric. The unknown constants
appearing in the solution are evaluated for the compact star PSR~J 1614-2230
for different values of coupling constant. The physical properties of the
model, e.g., matter density, pressure, stability etc. have been discussed both
analytically and graphically. This analysis showed that the geometry and matter
are compatible with each other as well as the model is in stable equilibrium in
the context of $f(R,\,T)$ modified gravity.
