  The pulsating eclipsing binaries are remarkable systems that provide an
opportunity to probe the stellar interior and to determine the fundamental
stellar parameters precisely. Especially the detached eclipsing binary systems
with (a) pulsating component(s) are significant objects to understand the
nature of the oscillations since the binary effects in these systems are
negligible. Recent studies based on space data have shown that the pulsation
mechanisms of some oscillating stars are not completely understood. Hence,
comprehensive studies of a number of pulsating stars within detached eclipsing
binaries are important. In this study, we present a detailed analysis of the
pulsating detached eclipsing binary system AI Hya which was studied by two
independent groups with different methods. We carried out a spectroscopic
survey to estimate the orbital parameters via radial velocity measurements and
the atmospheric parameters of each binary component using the composite and/or
disentangled spectra. We found that the more luminous component of the system
is a massive, cool and chemically normal star while the hotter binary component
is a slightly metal-rich object. The fundamental parameters of AI Hya were
determined by the analysis of binary variations and subsequently used in the
evolutionary modelling. Consequently, we obtained the age of the system as 850
$\pm$ 20 Myr and found that both binary components are situated in the Delta
Scuti instability strip. The frequency analysis revealed pulsation frequencies
between the 5.5 - 13.0 d$^{-1}$ and we tried to estimate which binary component
is the pulsating one. However, it turned out that those frequencies could
originate from both binary components.
