  As the global magnetic field of the Sun has an activity cycle, one expects to
observe some variation of the dynamical properties of the flows visible in the
photosphere. We investigate the flow field during the solar cycle by analysing
SDO/HMI observations of continuum intensity, Doppler velocity and longitudinal
magnetic field. We first picked data at disk center during 6 years along the
solar cycle with a 48-hour time step in order to study the overall evolution of
the continuum intensity and magnetic field. Then we focused on thirty 6-hour
sequences of quiet regions without any remnant of magnetic activity separated
by 6 months, in summer and winter, when disk center latitude B0 is close to
zero. The horizontal velocity was derived from the local correlation tracking
technique over a field of view of 216.4Mm x 216.4Mm located at disk center. Our
measurements at disk center show the stability of the flow properties between
meso- and supergranular scales along the solar cycle. The network magnetic
field, produced locally at disk center independently from large scale dynamo,
together with continuum contrast, vertical and horizontal flows, seem to remain
constant during the solar cycle.
