  The evolution of the inner accretion flow of a black hole X-ray binary
(BHXRB) during the outburst is still a matter of active research. X-ray
reverberation lags are powerful tools to constrain the disk-corona geometry. We
present a study of X-ray lags in the black hole transient H1743-322. We
compared results obtained from the analysis of all the publicly available
XMM-Newton observations. These observations were carried out during two
different outbursts, happened in 2008 and 2014. During all the observations the
source is caught in the hard state and at similar luminosities
($\mathrm{L_{3-10\ keV}/L_{Edd}\sim 0.004}$). We detected a soft X-ray lag of
$\sim$60 ms, most likely due to thermal reverberation. We did not detect any
significant change of the lag amplitude among the different observations,
indicating a similar disk-corona geometry at the same luminosity in the hard
state. On the other hand, we observe significant differences between the
reverberation lag detected in H1743-322 and in GX 339-4 (at similar
luminosities in the hard state), which might indicate variations of the
geometry from source to source.
