Excess energy and momentum deposition into the Earth's magnetosphere owing to the invasion of solar wind outbursts arising from active regions of the Sun causes major disturbances in the geomagnetic field referred to as geomagnetic storms (GMSs) (D'ujanga et al., 2013). The main drivers of GMSs are solar flares, coronal mass ejections (CMEs), and fast wind streams from coronal holes or their interplanetary remnants known as the interplanetary coronal mass ejections (Rawat et al., 2010;Richardson et al., 2006). The occurrence of GMSs is marked with a larger southward pointing interplanetary magnetic field (IMF), B z < −10 nT, that sustain for a period of time approximately longer than 3 h (Gonzalez & Tsurutani, 1987;Gonzalez et al., 1994). Southward B z is quite essential as it facilitates the transfer of energy, mass, and momentum from the solar wind into the Earth's magnetosphere through the magnetic reconnection with the northward directed geomagnetic field around Earth's magnetopause (Dungey, 1961).The state of the ionosphere at times of GMSs, commonly named ionospheric storms, describes variations of ionospheric parameters such as electron density, total electron content (TEC), or critical frequency (f o F 2 ) in response to geomagnetic storms. Based on the storm-induced alterations of the ionospheric parameters the ionospheric storms can be categorized as positive/negative corresponding to an increase/decrease in ionospheric parameters (