## 1 Introduction  
The formation of ionospheric plasma irregularities induces ionospheric scintillations, significantly affecting radio signals traversing the ionosphere. This phenomenon has substantial implications for the functionality of satellite navigation systems and radio communications, particularly for L-band radio signals, causing disturbances in both amplitude and phase, termed phase and amplitude scintillations [1, 2, 3]. Amplitude scintillations are quantified through the carrier-to-noise ratio (C/N0), measuring intensity variations, while phase scintillations involve assessing oscillations in the signal carrier phase [4; 5]. The behavioral analysis of ionospheric irregularities is complex, encompassing spatiotemporal variations and the influence of ionospheric layers, solar activities, and the interplanetary magnetic field (IMF). These factors serve as principal contributors to ionospheric disturbances across diverse geographical latitudes, with low latitudes posing unique challenges due to their direct connection to solar wind and magnetospheric disturbances [6]. Equatorial plasma bubbles (EPBs) represent a notable factor in ionospheric scintillations, characterized by large-scale disturbances aligned with the Earth's magnetic field. EPBs lead to a reduction in ionospheric plasma density, particularly in the lower F-layer near-equatorial regions, with the Earth's magnetic field playing a significant role [7]. The prevalence of this phenomenon is heightened within the equatorial ionospheric anomaly, situated approximately 15-20 degrees from the magnetic equator in low-latitude areas with elevated electron density [8]. Initiated by \(E\times B\) upward vector motion, equatorial plasma bubbles expand northward and southward from the equator, causing severe irregularities within the equatorial ionospheric anomaly. This process, characterized by a depleted plasma interacting with denser surrounding plasma, establishes a powerful gradient in the ionospheric structure, resulting in heightened ionospheric scintillations within the equatorial ionospheric anomaly [9]. In regions proximate to the equatorial ionospheric anomaly, around sunset, the vertical motion speed of ionospheric layers experiences an increment. Consequently, this leads to an elevation of the F-layer, subsequently causing an increase in the gradient of lower ionospheric layers. As a result, the level of equatorial plasma instability, referred to as Spread-F, undergoes enhancement [10]. Influential factors on Spread-F include solar cycles, seasonal variations, and local time dependencies. Moreover, the likelihood of Spread-F occurrence is strongly dependent on the geographical latitude of the region. It can be observed that the percentage of occurrence and the characteristics of this phenomenon are considerably variable and different in regions with lower latitudes compared to those at higher geographical latitudes. Regions with lower geographical latitudes typically exhibit more spread-F during the night, near sunset, and in the vicinity of the equinoxes [11]. Ionospheric disturbances occurring in the expanded F-layer region near the equator are a principal factor in the occurrence of ionospheric scintillations, known as Equatorial Spread-F (ESF). ESF events, with varying dimensions ranging from tens to hundreds of kilometers, occur in the magnetic equatorial region. The primary cause of these disturbances is an unstable process known as Rayleigh-Taylor instability, resulting from the vertical motion speed of ionospheric layers and an increase in the gradient of ionospheric layers in the equatorial anomaly region [12]. One of the most significant outcomes of Rayleigh-Taylor instability is the increased vertical plasma speed in the equatorial region, influenced by the background electric field of the magnetic equator [11]. Around sunset, an increase in the local electric field, known as the pre-reversal enhancement electric field (PRE), is observed, creating favorable conditions for the growth of Rayleigh-Taylor instability [13].