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We explore spectral properties of a Two-Component Advective Flow (TCAF)around a neutron star. We compute the effects of thermal Comptonization of softphotons emitted from a Keplerian disc and the boundary layer of the neutronstar by the post-shock region of a sub-Keplerian flow, formed due to thecentrifugal barrier. The shock location $X_s$ is also the inner edge of theKeplerian disc. We compute a series of realistic spectra assuming a set ofelectron temperatures of the post-shock region $T_{CE}$, the temperature of thenormal boundary layer (NBOL) $T_{NS}$ of the neutron star and the shocklocation $X_s$. These parameters depend on the disc and halo accretion rates($\dot{m_d}$ and $\dot{m_h}$, respectively) which control the resultantspectra. We find that the spectrum becomes harder when $\dot{m}_h$ isincreased. The spectrum is controlled strongly by $T_{NS}$ due to its proximityto the Comptonizing cloud since photons emitted from the NBOL cool down thepost-shock region very effectively. We also show the evidence of spectralhardening as the inclination angle of the disc is increased.

Monte Carlo Simulations of Thermal Comptonization Process in a Two Component Advective Flow around a Neutron Star