  We carry out detailed photometric and kinematic study of the poorly studied
sparse open clusters SAI 44 and SAI 45 using ground based BVR$_{c}$I$_{c}$ data
supplemented by archival data from \textit{Gaia} eDR3 and Pan-STARRS. The
stellar membership are determined using a statistical method based on
\textit{Gaia} eDR3 kinematic data and we found 204 members in SAI 44 while only
74 members are identified in SAI 45. The average distances to SAI 44 and SAI 45
are calculated as 3670$\pm$184 and 1668$\pm$47 pc. The logarithmic age of the
clusters are determined as 8.82$\pm$0.10 and 9.07$\pm$0.10 years for SAI 44 and
SAI 45, respectively. The color-magnitude diagram of SAI 45 hosts an extended
main-sequence turn-off (eMSTO) which may be originated through differential
rotation rates of member stars. The mass function slopes are obtained as
-1.75$\pm$0.72 and -2.58$\pm$3.20 in the mass rages 2.426-0.990 M$_{\odot}$ and
2.167-1.202 M$_{\odot}$ for SAI 44 and SAI 45, respectively. SAI 44 exhibit the
signature of mass segregation while we found a weak evidence of the mass
segregation in SAI 45 possibly due to tidal striping. The dynamical relaxation
times of these clusters indicate that both the clusters are in dynamically
relaxed state. Using AD-diagram method, the apex coordinates are found to be
(69$\fdg79\pm0\fdg11$, -30$\fdg82\pm0\fdg15$) for SAI 44 and
(-56$\fdg22\pm0\fdg13$, -56$\fdg62\pm0\fdg13$) for SAI 45. The average space
velocity components of the clusters SAI 44 and SAI 45 are calculated in units
of km s$^{-1}$ as (-15.14$\pm$3.90, -19.43$\pm$4.41, -20.85$\pm$4.57) and
(28.13$\pm$5.30, -9.78$\pm$3.13, -19.59$\pm$4.43), respectively.
