  The solutions of the \textit{diffuse reflection finite atmosphere problem}
are very useful in the astrophysical context. Chandrasekhar was the first to
solve this problem analytically, by considering atmospheric scattering. These
results have wide applications in the modeling of planetary atmospheres.
However, they cannot be used to model an atmosphere with emission. We solved
this problem by including \textit{thermal emission effect} along with
scattering.Here, our aim is to provide a complete picture of generalized finite
atmosphere problem in presence of scattering and thermal emission, and to give
a physical account of the same. For that, we take an analytical approach using
the invariance principle method to solve the diffuse reflection finite
atmosphere problem in the presence of atmospheric thermal emission. We
established the general integral equations of modified scattering function
$S(\tau; \mu, \phi; \mu_0, \phi_0)$, transmission function $T(\tau; \mu, \phi;
\mu_0, \phi_0)$ and their derivatives with respect to $\tau$ for a thermally
emitting atmosphere. We customize these equations for the case of isotropic
scattering and introduce two new functions $V(\mu)$ and $W(\mu)$, analogous to
Chandrasekhar $X(\mu)$, and $Y(\mu)$ functions respectively. We also derive a
transformation relation between the modified S-T functions and give a physical
account of $V(\mu)$ and $W(\mu)$ functions. Our final results are consistent
with those of Chandrasekhar at low emission limit (i.e. only scattering). From
the consistency of our results, we conclude that the consideration of thermal
emission effect in diffuse reflection finite atmosphere problem gives more
general and accurate results than considering only scattering.
