Space Physics and Aeronomy, Ionosphere Dynamics and Applications. Группа авторов

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СКАЧАТЬ 1994; Hosokawa et al., 2011), dawnside polar cap arcs can show quasi‐periodic poleward motion regardless of the IMF (Shiokawa et al., 1996). While polar cap arcs are typically a quasi‐static structure with slow dawn‐dusk motion, those can also involve substantial antisunward motion similarly to polar cap patches. Such motion particularly occurs for arcs that are associated with lower energy (hundreds of eV) precipitation, and those arcs can actively interact with the nightside auroral oval (Nishimura et al., 2013a; Zou et al., 2015b). Such soft electron precipitation and large electric field also effectively heat plasma and create upflows (Perry et al., 2015).

3.4 NIGHTSIDE AURORAL OVAL

      Localized and transient structures in the nightside auroral oval (Fig. 3.2) are primarily driven by electromagnetic and precipitation energy from the magnetotail, and ionosphere observations are useful for highlighting magnetosphere‐ionosphere coupling processes. Here we focus on ionosphere processes, and related magnetosphere processes are described in the companion book (Nishimura et al., in preparation).

      Auroral arcs are one of the most common auroral features. Arcs typically have widths between several hundred m and tens of km (Knudsen et al., 2001; Partamies et al., 2010). Quasi‐static arcs are associated with inverted‐V electron precipitation (Stenbaek‐Nielsen et al., 1998), while arcs with vortical forms such as curls (~5 km wavelength along the arc; Hallinan & Davis, 1970) involve Alfvenic precipitation (Chaston et al., 2010). Quiet arcs at evening to premidnight hours are located within the large‐scale upward Region‐1 FAC (Wu et al., 2017). The most intense arc is typically located close to the Region‐1/Region‐2 FAC boundary (Ohtani et al., 2010; Coroniti & Pritchett, 2014), and fast azimuthal flow channels are also seen at this boundary (Archer et al., 2017). While the substorm growth phase arc can also be found near the same boundary (Marghitu et al., 2009; Jiang et al., 2012), the growth phase arc migrates into the downward Region‐2 FAC during the late growth phase, forming two or more upward FACs in the auroral oval (Nishimura et al., 2012; Motoba et al., 2015). Such multipolar FACs tend to occur near midnight associated with substorms (Wu et al., 2017).

      Arcs are associated with enhanced precipitation, FAC, and electric field, and those drive active ionosphere feedback. Heating by precipitation and electric field drives plasma upflows, and fast flows enhance recombination. Those processes result in dynamic density structures (Zettergren et al., 2014; Lynch et al., 2015). The Alfvén resonator associated with FACs also contributes to create smaller‐scale density structures (Cohen et al., 2013).

Poleward boundary intensifications (PBIs) are auroral brightenings along the poleward boundary of the auroral oval (Lyons et al., 1999). PBIs are more intense during geomagnetically active times but can occur at all levels of geomagnetic activity. PBIs involve intense broad‐band Alfvénic electron precipitation (Mella et al., 2011). Cluster spacecraft observations showed that a growth of PBI corresponds to enhanced Alfvénic precipitation and then quasi‐static inverted‐V precipitation (Hull et al., 2016). PBIs are often followed by equatorward‐moving auroral arcs emanating from them. Those are called auroral streamers to distinguish from more stable east‐west oriented arcs. PBIs and streamers are the ionospheric signature of flow bursts in the nightside plasma sheet (Lyons et al., 1999) and a wedge‐type current system, where streamers mark upward FACs on the duskward edge of flow bursts (Sergeev et al., 2004). Radar observations show that streamers are located along the duskward edge of flow channels, where flows are generally substantially faster than large‐scale background convection speed (Shi et al., 2012; Gallardo‐Lacourt et al., 2014a; Pitkanen et al., 2011; Gabrielse et al., 2018). Even during storm times, fast flow channels and structured FACs are found to be the dominant mode of nightside auroral convection during the storm main phase (Lyons et al., 2016a).

      The most prominent auroral structure is the auroral substorm. Details of a typical substorm auroral sequence are described by Akasofu (1964) and Voronkov et al. (2003). Substorm auroral onset is characterized by sudden brightening (initial brightening) of one of the growth‐phase auroral arcs within the equatorward portion of the auroral oval. Initial brightening involves wavy modulation of auroral intensity along the arc, called beads or rays depending on looking angles (Donovan et al., 2006). Beads are associated with intense flow oscillation (Hosokawa et al., 2013; Gallardo‐Lacourt et al., 2014b).

      During poleward expansion of the arc, numerous auroral streamers originate in the vicinity of the poleward expanding arc and propagate equatorward. Individual streamers are associated with an intense wedge‐type current system and are a major contributor to local magnetic bays in ground magnetic field (Lyons et al. 2013). Although individual streamers are localized, a number of streamers arise during the expansion phase, and create modulation of the large‐scale substorm current wedge (SCW) (Forsyth et al., 2014). Streamers are associated with intense flows and particle injections into the inner magnetosphere and thus intensify various types of auroral activity in the equatorward portion of the auroral oval and subauroral ionosphere (Henderson, 2013), including pulsating aurora (Nishimura et al., 2018b) and omega bands (Henderson et al., 2006; Nishimura et al., 2013b). Diffuse auroral patch formation during substorms (Shiokawa et al., 2014) could also be a process related to substorm injection. Such localized aurora corresponds to localized precipitation (Hargreaves et al., 2010), which in many cases involves wave‐particle interaction in the magnetosphere (Nishimura et al., 2010a). Most intense electrodynamics during substorms can be seen along the poleward expanding arc and in the head of the westward traveling surge (Opgenoorth et al., 1983; Fujii et al., 1994; Gjerloev & Hoffman, 2002). The surge transitions to a quasi‐steady hook‐shaped auroral arc in the premidnight sector. Its clockwise open‐loop structure is an optical manifestation of the flow shear around the Harang reversal (thus called Harang aurora; Nishimura et al., 2010b).

      There are also auroral substructures embedded in the phenomena mentioned above. Electron diffuse aurora involves small‐scale (< ~km) curls, filaments, and black aurora (Maggs & Davis, 1968; Stenbaek‐Nielsen et al., 1999). Pulsating auroral patches include substructures of some tens of km (Nishiyama et al., 2016). Those are considered to include kinetic plasma dynamics in the magnetosphere. Measurements of radio signal scintillation indicate that small‐scale density irregularities occur associated with aurora and high‐density plasma (van der Meeren et al., 2014, 2015; Jin et al., 2014), and irregularities are tightly coupled to auroral arc motion but with a slight time lag, suggesting instability processes associated with density gradient and flow shear (Mrak et al., 2018).

The studies mentioned above have documented properties of mesoscale aurora and flows structures, but mesoscale precipitation has been rather poorly characterized. Global imaging can detect only bright structures of > ~100 km size but attempts have been made to utilize ground‐based imaging to deduce precipitating electron fluxes by resolving individual auroral structures (Partamies et al., 2004; Grubbs et al., 2018). While their studies are limited to a single all‐sky imager, here we present an approach to use the THEMIS ASI array to cover a semicontinental scale, which is critical for account for the entire substorm region. Figure 3.3 shows 2‐D energy flux during a substorm at 7 UT on 26 March 2014. Technical details are beyond the scope of this chapter and will be reported more in detail elsewhere (Nishimura et al., 2018c) but, in brief, the THEMIS ASI data were used to convert white light images to red‐green‐blue colors by comparing to the nearest NORSTAR meridian scanning photometers, and then the color ratios were converted to energy fluxes and characteristic energies using the Rees and Luckey (1974) formulas. While the data were mapped to 110 km altitude, mapping and viewing angle effects provide uncertainties in interpretation of derived parameters.

Figure СКАЧАТЬ