  One of the most straightforward ways to explain the hard X-ray spectra
observed in X-ray binaries is to assume that comptonization of soft photons
from the accretion disk is occurring. The region where this process takes
place, called the corona, is characterized by only two parameters: its thermal
energy $kT$ and its optical depth $\tau$. Hard X-ray spectra analysis is, thus,
an imperative tool in diagnosing the behavior of these parameters. The lack of
consistency in obtaining/analysing long-term databases, however, may have been
hindering this kind of characterization from being attained. With the aim of
better understanding the corona behavior in the black hole candidate 1E
1740.7-2942, we performed a homogeneous analysis for a large hard X-ray data
set from the ISGRI telescope on-board the INTEGRAL satellite. Results from
modelling the spectra show that, for most of our sample, unsaturated thermal
comptonization is the main mechanism responsible for the hard X-ray spectra
observed in 1E 1740.7-2942. Moreover, such extensive database allowed us to
produce what is probably the longest hard X-ray light curve of 1E 1740.7-2942
and whose units -- due to recent findings regarding dynamical quantities of the
system -- could be expressed in % of Eddington's luminosity.
