  Three homologous C-class flares and one last M-class flare were observed by
both the Solar Dynamics Observatory (SDO) and the Hinode EUV Imaging
Spectrometer (EIS) in the AR 11429 on March 9, 2012. All the recurrent flares
occurred within a short interval of time (less than 4 hours), showed very
similar plasma morphology and were all confined, until the last one when a
large-scale eruption occurred. The C-class flares are characterized by the
appearance, at approximatively the same locations, of two bright and compact
footpoint sources of $\approx$~3--10~MK evaporating plasma, and a semi-circular
ribbon. During all the flares, the continuous brightening of a spine-like hot
plasma ($\approx$~10~MK) structure is also observed. Spectroscopic observations
with Hinode/EIS are used to measure and compare the blueshift velocities in the
\fexxiii\ emission line and the electron number density at the flare footpoints
for each flare. Similar velocities, of the order of 150--200~km~s$^{-1}$, are
observed during the C2.0 and C4.7 confined flares, in agreement with the values
reported by other authors in the study of the last M1.8 class flare. On the
other hand, lower electron number densities and temperatures tend to be
observed in flares with lower peak soft X-ray flux.In order to investigate the
homologous nature of the flares, we performed a Non-Linear Force-Free Field
(NLFFF) extrapolation of the 3D magnetic field configuration in the corona. The
NLFFF extrapolation and the Quasi-Separatrix Layers (QSLs) provide the magnetic
field context which explains the location of the kernels, spine-like and
semi-circular brightenings observed in the (non-eruptive) flares. Given the
absence of a coronal null point, we argue that the homologous flares were all
generated by the continuous recurrence of bald patch reconnection.
