  We performed a detailed timing study of the Atoll source 4U 1705-44 in order
to understand the accretion disk geometry. Cross correlation function (CCF)
studies were performed between soft (3-5 keV) and hard energy (15-30 keV) bands
using the AstroSat LAXPC data. We detected hard as well as soft lags of the
order of few ten to hundred seconds. A dynamical CCF study was performed in the
same energy bands for one of the light curves and we found smaller lags of few
tens of seconds ($<$ 50 s) suggesting that the variation is probably
originating from the corona. We found a broad noise component around $\sim$ 13
Hz in the 3-10 keV band which is absent in 10-20 keV band. We interpret the
observed lags as the readjustment timescales of the corona or a boundary layer
around the neutron star and constrain the height of this structure to few tens
of km. We independently estimated the coronal height to be around 15 km
assuming that the 13 Hz feature in the PDS is originating from the oscillation
of the viscous shell around the neutron star.
