Figure 2 shows the electron density (top row), meridional wind (middle row), and temperature (bottom row) at 250 km altitude for the location of Mt. Abu as simulated by WACCM-X for three sample days. On these three days, an increase in electron densities is seen after sunset which coincides with the reversal in meridional winds from equatorward to poleward direction. Enhancements in electron densities occur at 21, 23, and 21 LT, respectively, for the three given nights, and the meridional winds show a reversal in the poleward direction at that time. The variation in electron densities at 250 km shows a one-to-one relation with the OI 630.0 nm nightglow emissions for geomagnetic quiet time period, which has been established by the estimated OI 630.0 nm nightglow emissions, wherein the measured electron densities were used as inputs (Saha et al., 2021). Typically, the meridional winds turn equatorward after sunset, but interestingly, a reversal in equatorward wind is seen in the estimated relative variation in meridional winds for a period of 2-3 hours (Saha et al., 2021). The WACCM-X model also shows a similar reversal in meridional winds after sunset, as shown in Figure 2.