Context : Classical Be stars are hot non-supergiant stars surrounded by a gaseous circumstellar disk that is responsible for the observed infrared ( IR ) excess and emission lines .
The influence of binarity on these phenomena remains controversial .

Aims : We followed the evolution of the environment surrounding the binary Be star \delta Scorpii one year before and one year after the 2011 periastron to check for any evidence of a strong interaction between its companion and the primary circumstellar disk .

Methods : We used the VLTI/AMBER spectro-interferometric instrument operating in the K band in high ( 12000 ) spectral resolution to obtain information on both the disk geometry and kinematics .
Observations were carried out in two emission lines : Br \gamma ( 2.172 \mu m ) and { He \textsc { i } } ( 2.056 \mu m ) .

Results : We detected some important changes in \delta Scorpii ’ s circumstellar disk geometry between the first observation made in April 2010 and the new observation made in June 2012 .
During the last two years the disk has grown at a mean velocity of 0.2 km s ^ { -1 } .
This is compatible with the expansion velocity previously found during the 2001-2007 period .
The disk was also found to be asymmetric at both epochs , but with a different morphology in 2010 and 2012 .

Conclusions : Considering the available spectroscopic data showing that the main changes in the emission-line profiles occurred quickly during the periastron , it is probable that the differences between the 2010 and 2012 disk geometry seen in our interferometric data stem from a disk perturbation caused by the companion tidal effects .
However , taking into account that no significant changes have occurred in the disk since the end of the 2011 observing season , it is difficult to understand how this induced inhomogeneity has been “ frozen ” in the disk for such a long period .