  We compute the rate of change of mass and angular momentum of a black hole,
namely tidal heating, in an eccentric orbit. The change is caused due to the
tidal field of the orbiting companion. We compute the result for both the
spinning and non-spinning black holes in the leading order of the mean motion,
namely $\xi$. We demonstrate that the rates get enhanced significantly for
nonzero eccentricity. Since eccentricity in a binary evolves with time we also
express the results in terms of an initial eccentricity and azimuthal frequency
$\xi_{\phi}$. In the process, we developed a prescription that can be used to
compute all physical quantities in a series expansion of initial eccentricity,
$e_0$. These results are computed taking account of the spin of the binary
components. The prescription can be used to compute very high-order corrections
of initial eccentricity. We use it to find the contribution to eccentricity up
to $\mathcal{O}(e_0^5)$ in the spinning binary. We also provide an approximate
expression for $\mathcal{O}(e_0^n)$, where $n$ is any odd number. With this, we
compute approximate expression for $\mathcal{O}(e_0^7)$ and
$\mathcal{O}(e_0^9)$ for non-spinning binary. Using the computed expression of
eccentricity, we derived the rate of change of mass and angular momentum of a
black hole, both rotating and non-rotating, in terms of initial eccentricity
and azimuthal frequency up to $\mathcal{O}(e_0^6)$. We also compute leading
order dephasing in both cases analytically up to $\mathcal{O}(e_0^6)$ and study
its impact.
