A complex magnetic topology at Mars gives rise to diverging magnetic field cusps and closed magnetic loops with local magnetic conditions similar to those found above Earth’s polar region. One of such cusps is located at 82oS and 180oE where the crustal magnetic field is nearly vertical and open to the access of solar wind plasma through magnetic reconnection with the interplanetary magnetic field. This reconnection can allow solar wind electrons to penetrate into the Martian upper atmosphere, causing ionization and heating, which leads to inflate the topside plasma distribution to high altitude and increase the topside electron density scale height. These characteristics of the Martian upper atmosphere at this southern location are confirmed from the Mars Express electron density profile. We use our 1-D chemical diffusive model from an altitude of 100 km to 400 km to interpret the measured electron density profile with the vertical plasma transport simulated by vertical ion velocities and by imposing an outward flux boundary condition. The output of this model and available crustal magnetic field information at Mars are used to estimate the vertical distribution of ionospheric conductivities. We find that the ionosphere is highly conductive in the Martian dynamo region between 100 and 250 km altitude where plasma –neutral collisions permit electric currents perpendicular to the crustal magnetic field. The magnitudes of Pedersen and Hall conductivities are estimated to be ~0.01 – 0.075 S/m, respectively, near the Martian ionospheric peak. We also estimated the magnitude of horizontal ionospheric currents driven by ion and electron motions in the Martian dynamo region. The model results will be presented in comparison with existing estimates of the Martian conductivities and ionospheric currents.. The research reported in this poster is supported by Mohammed Bin Rashid Space Centre (MBRSC), Dubai, UAE, under Grant ID number 201604.MA.AUS.