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Simultaneous ground-based optical and SuperDARN observations of the shock aurora at MLT noon
© Liu et al. 2015
- Received: 21 December 2014
- Accepted: 8 July 2015
- Published: 29 July 2015
Using ground-based high temporal and spatial optical aurora observations, we investigated one fortuitous event to illustrate the direct responses of the fine structure auroral emission to interplanetary shock on 7 January 2005. During the shock impact to the magnetosphere, the Chinese Arctic Yellow River Station (YRS) equipped with all-sky imagers (ASIs) was situated at the magnetic local noon region (~1210 MLT) in the Northern Hemisphere, while the SuperDARN CUTLASS Finland HF radar covering the field of view (FOV) of the ASIs at YRS had fine ionospheric plasma convection measurement. We observed that an intensified red aurora manifesting as a discrete emission band at a higher latitude responds to the shock impact gradually, which results in a distinct broadening of the dayside auroral oval due to the equatorward shifting of its lower latitude boundary after the shock arrival. In contrast, the green diffuse aurora, manifesting as a relatively uniform luminosity structure, reacts immediately to the shock compression, displaying prompt appearance in the southern edge of the FOV and subsequent poleward propagation of its higher latitude boundary. Simultaneously, the CUTLASS Finland radar monitored enhanced backscatter echo power and increased echo number, which coincided with intensified discrete aurora in approximately the same latitudinal region. Doppler velocity measurement showed moving ionospheric irregularities with generally enhanced line-of-sight (LOS) speed, but with prominent sunward flow in the polar cap and antisunward flow in both the eastern and western regions. The SuperDARN global ionospheric convection pattern clearly presented a large-scale plasma flow divided in four circulation cells, with two reversed flow cells nested in the noon sector of the polar cap. These direct observations strongly suggest that the prompt shock compression intensified the wave-particle interaction in the inner magnetosphere and enhanced the lobe magnetic reconnection rate at magnetospheric high latitude.
- Interplanetary shock
- Sudden impulse
- Optical aurora
- Sunward flow
The large-scale auroral feature associated with interplanetary shock (i.e., shock aurora) has been investigated widely over the last two decades mainly using satellite onboard imager observations (Sibeck et al. 1999; Zhou and Tsurutani 1999; Zhou et al. 2003; Meurant et al. 2003; Meurant et al. 2005). It is well known that shock aurora imaged from satellites show that the general auroral emission brightens near local noon region at the time of the shock arrival to the magnetopause nose. The initial brightening sector of shock aurora was usually limited to the ionospheric footprint of the magnetospheric cusp with longitudinal width of a few magnetic local time (MLT) hours, and then propagates toward dawnside and duskside along the auroral oval flanks with high speed and terminates the midnight sector ultimately (Zhou and Tsurutani 1999; Tsurutani et al. 2001; Meurant et al. 2004). The magnetospheric cusp is a region in which the magnetosheath plasma has direct access to the polar ionosphere, and is the first region to directly respond to IP shocks in geospace (Fuselier et al. 2000; Zhou et al. 2009). Therefore, detailed studies focusing on the shock-related phenomena in the cusp, especially around the MLT noon, are quite essential in revealing its early response.
Previous studies on shock aurora were mainly concentrated on the measurements of large-scale auroral emissions from satellite imager observations and characteristics of energetic particle precipitation, but with few works using ground-based medium and small-scale optical aurora and simultaneous related ionospheric plasma drift measurements (Zhou and Tsurutani 1999; Zhou et al. 2003; Meurant et al. 2003; Zhou et al. 2009; Motoba et al. 2009; Liu et al. 2011). It is known that large-scale auroral imaging benefits to reveal the overall interaction process during this critical condition affected by the disturbed solar wind structure, but detailed ground-based measurement also plays an essential role in understanding the fine interaction inside the compound coupling system. It is generalized that, however, overall features on the oval and some localized aurora beyond the oval were captured visually and analyzed with the aim to study how the solar wind affects the magnetosphere globally through changes in the Earth's aurora (Zhou et al. 2003; Hubert et al. 2003; Hubert et al. 2006; Frey 2007; Hubert et al. 2013).
Aurora responding to the IP shock compression or the sudden solar wind dynamic pressure enhancement from ground-based optical measurement revealed that the intensified diffuse and discrete aurora expanded equatorward (Sandholt et al. 1994; Zhou et al. 2009). Based on simultaneous ground-satellite optical observations in the Southern Hemisphere, Motoba et al. (2009) revealed a two-step development of the postnoon shock aurora, which shows first diffuse aurora expanding duskward at the equatorward edge of the oval and subsequent newly formed discrete arcs in the middle of the oval. Afterwards, Liu et al. (2011) reported a transient decrease of discrete aurora and simultaneous ionospheric plasma flow reversal for short period just after the shock arrival, i.e., during the preliminary impulse of a sudden commencement event. Intensified auroral arc with a lifetime of ~14 min and periodical oscillation in the ionospheric plasma flow were detected by ASI and SuperDARN caused by the shock impact (Liu et al. 2013). All of these works mentioned above demonstrated that more features of shock aurora and related ionospheric response have not been unveiled yet. Most studies associated with shock-related aurora specialized in research on variation of the 630.0-nm red discrete aurora as a proxy for the open-close field line boundary (Sandholt et al. 1994; Blanchard et al. 1995; Blanchard et al. 1997), but they do not pay more attention to the detailed variation of diffuse auroral emission around MLT noon. Therefore, a general direct relationship between dayside aurora and IP shock has been observed, but more exact response time and certain auroral forms have been elusive because of low temporal and spatial resolution observation.
It is well known that the interplanetary shock plays a key role on magnetospheric configuration (Boudouridis et al. 2003; Laundal and Østgaard 2008). It follows that such influence over the magnetospheric configuration will have a corresponding effect on the size and location of the auroral oval, polar cap, and the associated auroral intensity, field-aligned currents, and ionospheric convection (Boudouridis et al. 2007). Coco et al. (2008) used SuperDARN, spacecraft and ground magnetometer data to study the magnetosphere compressed by an interplanetary shock during an IMF By-dominated period, they found that at very high latitudes above the northern cusp and in the morning sector, enhanced sunward convection fluxes appear with a signature typical for northward Bz-dominated lobe reconnection.
YRS produces high quality optical data and is ideally located to monitor the dayside aurora (Hu et al. 2009; Zhang et al. 2010). We checked one shock aurora event with high temporal and spatial resolution when YRS was located around MLT noon, which gives us an opportunity to make more detailed examination of the evolution of visible auroral emissions (green and red) during the disturbed magnetosphere caused by the external shock impact. Furthermore, the SuperDARN CUTLASS Finland radar, which is a stereo system with two experimental modes and scans over the YRS (Lester et al. 2004), has full ionospheric irregularity monitoring results. Those combined measurements enabled us to extend our view to shock aurora fine structure and its related ionospheric signature.
To address how ionospheric convection responds to the shock compression, we checked the SuperDARN radar observation in the Northern Hemisphere. CUTLASS (Co-operative UK Twin Located Auroral Sounding System) Finland HF radar, located at Hankasalmi (62.3° N, 26.6° E) and operated since February 1995, is an essential part of the SuperDARN radar network (Lester et al. 2004; Chisham et al. 2007). It has an array of 16 transmitting and receiving antennas. The radar can operate at frequencies between 8 and 20 MHz in the HF band, and each antenna array is phased relative to the others to form an antenna pattern with maximum gain in one of the 16 azimuthal pointing directions (so-called beams). The beam width is set to ~3.4°; thus the CUTLASS Finland radar has roughly 54° azimuthal FOV coverage with its central beam scanning over zenith of YRS as shown by radial solid line in Fig. 1.
The coherent CUTLASS Finland radar measures ionospheric backscatter echoes from field-aligned plasma irregularities in the high-latitude ionosphere (Lester et al. 2004). These backscatter Doppler echoes can be used to derive parameters of echo power, line-of-sight velocity, and spectral width. With regard to this study, the CUTLASS Finland radar was operating in a frequency of 11 MHz and scanned 16 beams with a dwell time of 7 s at each beam, giving a fan-shaped FOV scanning every 2 min. For each beam, a total of 75 range gates were sampled with a pulse length of 300 us, corresponding to a range gate length of 45 km. The time lag to the first gate was set at 1200 us, which means that the range was extended from 180 to 3555 km for one beam. Consequently, YRS at NYA formed a better place for investigating the auroral fine structure and simultaneous ionospheric plasma convection.
Solar wind and geomagnetic field response
Optical auroral data
Before the SI onset at ~09:22 UT, Fig. 4 shows that the dim green aurora in ray or weak patchy structure can be seen in the northern portion of the FOV, which signifies that the cusp auroral emission was steady before ~09:22 UT, namely intervals prior to the magnetospheric disturbance caused by the shock impact. It is worth noting that southern unstructured, quite low, intensity emissions at ~0.25 kR were detected by the ASI. This fundamental optical signature in the southern portion of the FOV of the ASI signifying the wave-particle interaction did not show active in the inner magnetosphere as it can be expected from the low geomagnetic activity manifesting as stable Sym-H index shown in Figs. 2 and 3 (Ni et al. 2008; Chen et al. 2012). Clear response of the green line emission to the shock prompt compression started instantly at the SI onset time of 09:22:00 UT, which was first illuminated diffuse aurora with fairly uniform luminosity in the southern sky, as shown in Fig. 4 by an oblique downward black arrow. This arrow in the 09:22:00 UT frame of Fig. 4 points the preliminary and instantaneous brightened diffuse aurora just after the SI onset. Shortly afterwards, it is shown that those intensified uniform diffuse aurora propagated to the high-latitude region expeditiously under continuous compression, and this noticeable brightened diffuse aurora was widespread over the entire sky at 09:23:40 UT (not shown). After reaching its maximum brightness at 09:24:30 UT, the diffuse aurora observed near the center of the FOV of the ASI shrank gradually back to the southern portion of the image and propagated eastward with decreasing brightness. This phenomenon evidently indicates that the unstructured diffuse precipitation associated with the inner magnetospheric wave-particle interaction processes first occurred at lower latitude caused by the shock prompt compression. Thereafter, the poleward boundary of diffuse aurora spreads to the higher latitude within very short time period as shown in Fig. 4. Here we used the high photosensitive and spatiotemporal resolution images to detect the diffuse auroral emissions during the shock compression. As a consequence, the response time of the diffuse aurora inferred from those corresponding auroral images is known with an accuracy of ~10 s, i.e., the time resolution that stems from the imaging cadence.
SuperDARN radar observation
In the middle plots of Fig. 7, reddish color represents the plasma flow of ionospheric irregularities away from the radar, and the flow toward the radar was denoted by greenish color. The figure at 09:20:00 UT shows that LOS velocity has a sunward component less than 200 m/s in the west part of the FOV and presents weak antisunward flow in the center of the echo band (across the polar cap). After the SI onset, the LOS velocity shows plasma flow with dominantly higher speed \away from the radar (antisunward) in the eastern region, whereas toward the radar (sunward) in the west region. A striking feature of the ionospheric plasma convection in the local noon sector is the enhanced sunward flow just after the shock impact on the terrestrial magnetosphere. Furthermore, it is indicated that ionospheric plasma irregularity structure propagated eastward under close scrutiny after comparison between scans before and after the SI. At 09:25:00 UT, Fig. 7 shows that the plasma flows were away from the radar both in the eastern and western portion but with noticeable sunward flows in center beams.
The Doppler spectral width shown in the bottom panels of Fig. 7 was narrow (<200 m/s) and backscatter coverage was poor before the shock arrival, but it became wider (>250 m/s) and extended in latitudinal after the SI onset was triggered by the shock. Figure 7 shows that the latitudinal profiles of Doppler spectral width displays a typical pattern of high spectral widths at high latitudes and low spectral widths at low latitudes. Actually, multi-instrumentation observations showed that the equatorward boundary of the high latitude Doppler spectral width can be interpreted as co-locating with the open-/closed-field line boundary (Milan et al. 1999). Concerning the present SuperDARN observations, the spectral width boundary around ~77°, MLAT is a good proxy for the open/closed-field line boundary, especially when the SuperDARN radar is located around the geomagnetic local noon sector (Chisham et al. 2007). Both enhanced spectral width and its equatorward moving signify that the footprint of the equatorward boundary of the cusp propagated southward after the sudden shock compression.
The fine structure dayside aurora response to prompt IP shock compression has recently been investigated by, for instance, by Zhou et al. (2009) and Motoba et al. (2014). The auroral response near local noon has been reported using meridian scanning photometer and 30-s ASIs data. Sandholt et al. (1994) firstly revealed that strong and isolated enhancements in solar wind dynamic pressure gave rise to equatorward shifts of the cusp/cleft aurora, characteristic auroral transients, and distinct ground magnetic signatures of enhanced ionospheric plasma convection at cusp latitudes. Zhou et al. (2009) studied dayside shock auroral forms and their variations when Svalbard was at ~1120 MLT, and they found that both green and red auroral emissions intensified by a factor larger than 2 within 5 min after the shock arrival to the magnetosphere, equatorward and eastward expanding diffuse aurora on closed-field lines and doubled the cusp meridional width due to equatorward motion of the low latitude boundary of the cusp.
In the present event, we concentrate on the detailed evolution of the diffuse and discrete aurora by using high temporal and spatial ground-based optical observation and simultaneous ionospheric plasma drift determined with the SuperDARN radar located at Hankasalmi during the interval following the IP shock compression of the magnetosphere. Here we note that ground-based optical aurora and simultaneous ionospheric convection observed during the shock compression under weakly northward IMF conditions differ from previous observational results. Just after the SI onset triggered by the impinging IP shock, fainter and fairly uniform luminosity structure of diffuse-type aurora first appeared in the southern sky of the FOV of the ASI. Subsequently, the intensified diffuse aurora propagated poleward expeditiously, as illustrated in Fig. 4. This instant response of diffuse-type aurora to the impinging IP shock is similar with the immediate geomagnetic field variation shown in Fig. 3. To our knowledge, this southward initial appearance and extreme fast poleward-moving medium-diffuse aurora subsequently in the midday sector associated with shock compression or increased solar wind dynamic pressure was rarely noticed in related literature, except for the studies of Shi et al. (2012) and (Chen et al. 2012). Moreover, it is found that those diffuse auroras spread across the full FOV of the ASI in a very short time period (~2 min). In addition, concurrent gradual equatorward moving of lower latitude boundary of discrete auroral band brightened in the higher latitude region and typical bursts reversed convection in local noon polar cap are another significant ionospheric dynamical phenomenon within compressed magnetosphere.
Diffuse aurora is primarily caused by the precipitation of energetic electrons (0.1–30 keV) in the atmosphere along the magnetic field lines, and occurs over a broad latitude range (Ni et al. 2008; Thorne et al. 2010). Although generally not visible by naked eyes, the diffuse auroral precipitation provides the main energy source for the high-latitude upper atmosphere (Newell et al. 2009). Concerning the present event, the IMF Bz was primarily dominated by positive value (northward orientation), and the solar wind condition was relatively quiet before the sudden enhancement of the solar wind dynamic pressure indicated in Fig. 2, thus the magnetosphere was nearly undisturbed before the SI onset due to the inefficiency of energy loading from the solar wind to the magnetosphere by component magnetic reconnection in the low-latitude magnetopause (Fuselier and Lewis 2011). The extremely faint diffuse-type auroral structure flickering in the southern edge of the FOV of the ASI at YRS shown in Fig. 4 was also a good indicator for the quiet magnetospheric circumstance. We note that when the magnetosphere was impinged by the IP shock, the magnitude of the geomagnetic field clearly increased at lower latitude (Fig. 3). This can be understood in terms of an enhancement of the magnetopause current flowing from dawnside to duskside as the compressional wave approaches. It was previously shown that VLF chorus wave activity in the magnetospheric cavity can be triggered or see its intensity increased while the energetic electron precipitation is enhanced significantly and rapidly as well, as a result of the sudden external compression by the IP shock (Gail et al. 1990). Consequently, the wave-particle interaction properties are significantly affected by the magnetic perturbation and plasma variations associated with a shock sudden impact.
As discussed by Zhou et al. (2003), an approaching fast-moving forward shock compresses the magnetosphere, leading to a smaller cavity by moving the magnetopause earthward, which consequently increases the magnetic field. Both effects produce a heating of the plasma in the perpendicular direction and increases the temperature anisotropy under the assumption of the conserved first adiabatic invariant. The loss cone instability will occur and subsequently result in plasma wave growth, such as whistler mode chorus waves mentioned above. It is known that the increasing instability of plasma wave is capable of causing pitch angle scattering and has the strongest growth at the equator plane (Zhou and Tsurutani 1999). Thus, the waves are the most intense near the equatorial plane. The instability grows after the SI onset and wave-particle interactions subsequently produce abundant electron precipitation. Those electrons entering the loss cone due to the adiabatic compression will precipitate along the geomagnetic field lines into the polar atmosphere and uniformly distribute in large area (Tsurutani et al. 2001). The precipitating particles with enhanced energy flux collide with the atmospheric atoms and molecules, producing unstructured diffuse-type aurora with no sharp structure as shown in Fig. 4. We thus interpret the fast poleward-moving signature presented in Fig. 4 as the result of the onset of energetic electron-wide falling, rather than as a material motion.
Ground-based optical aurora observation showed that the interplanetary shock compression caused prominent diffuse aurora responding both in moving feature and increased intensity. The enhanced green aurora was mainly diffuse aurora in the southern sky. It is believed that the bounce periods for energetic electrons and ions of ~1–10 keV between Northern and Southern hemispheres at ~75°; MLAT are seconds and minutes, respectively (Tsurutani et al. 2001; Zhou et al. 2009). So after compression, preexisting particles should be lost after ~10 s or min (Tsurutani et al. 2001). Here, the optical aurora data with very high time resolution at 10 s per image is quite essential for determining the response time of shock aurora. By examining the diffuse auroral sequential images presented here, the response time of the green diffuse aurora at MLT noon to the sudden shock compression as deduced from our optical observation is smaller than 10 s, which is greatly significant for understanding the solar wind-magnetosphere dynamical coupling process under extreme space environment.
The red line emission appearing as discrete elongated auroral band in Fig. 5 shows different spatial and temporal variations compared with simultaneous observation of the diffuse-type aurora in green line emission. In this event, the IMF had predominantly a positive Bz (northward IMF) and minor negative By component before the arrival of the shock disturbance structure to the ACE satellite shown in Fig. 2. This kind of IMF condition was corresponding to the unusual optical auroral activity at the higher latitude region (referred as type 2 cusp aurora by (Øieroset et al. 1997)), such as the dayside corona of aurora shown in Fig. 5. Because of the quiet geomagnetic activity due to the smooth solar wind parameters shown in Fig. 2 before the SI onset, dayside discrete aurora had continuous and steady weak emission over the magnetic latitudinal range from ~78.5° to ~79.8° for a long time, referred to as red auroral keogram in Fig. 6b. Just when the fast-moving forward shock front arrives, simultaneous IMF Bz had a minor excursion for a very short interval preceding the following northward IMF. This solar wind disturbance propagated to Earth space and triggered clear and enhanced geomagnetic perturbation subsequently denoted by the prompt increased Sym-H index plotted in the bottom panel of Fig. 3.
Figure 5 illustrates that the response of the discrete aurora to the shock compression was a gradual process in either auroral form or emission intensity. From 09:22:00 to 09:23:40 UT, the discrete red aurora in the high-latitude region did not present evident spatial and temporal variation in the main auroral oval compared with the rapid poleward motion of the diffuse aurora in the southern sky just after the SI onset shown in Fig. 4. Just weak enhanced discrete auroral bifurcation formed at eastern part of the emission band during preliminary phase of the SI, which was marked by the black arrow in the frame at 09:22:00 UT. As time went by, noticeable features of the discrete aurora commenced at 09:23:50 UT (under detailed examination, but not shown here) in response to the shock squeezing of the magnetosphere, which was identified as the intruding optical filaments in the central portion of the FOV of the ASI with substantial equatorward displacement of the observed structures seen in the auroral 10 s sequential frames. Therefore, the lower latitude edge of the emission band shifted equatorward in the magnetic latitude range from ~78.5° to ~76.9° approximately around 09:30:00 UT. As a reliable proxy for the polar cap boundary, the poleward boundary of the red emission band did not experience obvious spatial motion during the external compression (Blanchard et al. 1995; Lester et al. 2001). Clearly, the width of the emission band broadens certainly due to the equatorward expansion of the auroral structure observed in the lower latitude portion, which appears in Fig. 6b as a variation of the auroral width and an enhancement of the intensity.
As the visible feature of the aurora on the dayside red-dominated, the 557.7-nm green line emission is due to the transition of an electron from the 1 S excited state to the 1 D state of atomic oxygen. Another commonly observed line, particularly in the polar cusp and cap, is the red line at 630.0 nm as the 1 D state relaxes to the ground state (Carlson and Egeland 1995). As presented in the current study, the diffuse aurora in the FOV of the ASIs only detected in green line emission was brightened in the lower latitude at the beginning of the SI, and then experienced fast poleward motion. While discrete aurora was also observed in the north zenith of the YRS and displayed as rayed sharp beam structures as shown in Fig. 4. A precipitation model, which separately categorizes two types of discrete precipitation (monoenergetic and broadband spectra) and both electron and ion diffuse precipitation, was developed by Newell et al. (2009). It allowed a quantitative comparison between four types of precipitation. The results turn out that the diffuse aurora is surprisingly dominant, constituting 84 % of the energy flux into the ionosphere during conditions of low solar wind driving (63 % electrons, 21 % ions), and is more dynamic, rising rapidly with increasing solar wind driving. By using DMSP observation, Newell and Meng (1992) found that soft electron precipitation (0.1–1 keV) dominates discrete aurora, and spectral flux is higher in the closed-field line region. Moreover, it is known that enhanced wave-particle interaction in equatorial magnetosphere transiently responds to the external sudden compression (Gail et al. 1990; Shi et al. 2012). Therefore, diffuse aurora is more prominent than discrete aurora in 557.7 nm emission as shown in Fig. 4 just after the external sudden compression.
It is well known that the high-latitude discrete aurora is closely related with the physical processes occurring around the magnetopause where the IMF and terrestrial magnetic field line can reconnect under certain dynamical conditions (Sandholt et al. 1996; Øieroset et al. 1997). Here, a discrete aurora occurred as elongated emission band in the far poleward portion of the FOV of the ASI at YRS. Its location corresponds well to the ionospheric backscatter echoes monitored by the SuperDARN radar located at Hankasalmi. Based on the coordinated ground-based optical aurora data at 630.0 nm and equivalent convection maps deduced from magnetometer observations, Sandholt et al. (1996) suggested that the high-latitude discrete aurora situated at ~77°–78°, MLAT corresponds to injections of magnetosheath plasma associated with magnetic reconnection between the IMF and the lobe magnetic field tailward of the cusp in the high-latitude magnetopause. Concerning the present event, the equatorward-moving auroral filaments close to right zenith of YRS are marked by the oblique white arrow in Fig. 5 was a potential signature of lobe reconnection associated with sudden shock squeezing.
Under northward IMF condition, the interplanetary field lines drape over the magnetopause such that the orientation of the IMF is antiparallel to that of the open-lobe field lines tailward of the cusp. Magnetic reconnection takes place between the interplanetary magnetic field line and the geomagnetic field line, and in most cases the result is a field line draped on the dayside magnetopause with one footprint in the Northern or Southern hemisphere, and a detached field line on the nightside that is eventually carried away by the high speed solar wind stream. A combination of the magnetic tension force on the bent field line and the flow of the solar wind past the Earth results in the footprint of the field line being dragged initially sunward. Since it has remained open, it stays within the region of open field lines within the auroral oval, namely, the polar cap, and does not cross the open/closed-field line boundary (Imber et al. 2006). The field line then slips around the side of the magnetosphere and then is added to the magnetotail lobe. Therefore, the ionospheric convection pattern under northward IMF condition becomes quite complex, consisting of either distorted two cells or multiple cells rather than the common two-cell large-scale circulation pattern with dawn cells in counter-clockwise circulation and reverse polarity circulation in the dusk cell. In the case of a multicell pattern, the flows are expected to form two “reverse” convection cells in the noon sector of the polar cap with clockwise circulation on the prenoon sector and counter-clockwise circulation on the postnoon region, respectively. Correspondingly, plasma that flows across the central polar cap are sunward instead of antisunward.
Here, intruding discrete auroral filaments observed after the shock squeezed the magnetosphere should be considered one possible ionospheric signature of the lobe reconnection associated with ionospheric convection variation. Actually, the CUTLASS Finland radar scanning toward the polar cap in the local noon sector detected obvious sunward plasma flow in far range gates after the shock arrival, which was described above and also shown in both Fig. 7 and Fig. 8. Furthermore, much more ionospheric backscatter echoes reflected by plasma irregularities aligned along the geomagnetic field lines were monitored by this radar, and these echoes gradually moved equatorward as seen after a closer scrutiny. To verify whether or not lobe reconnection occurred during shock compression, we check the global ionospheric convection pattern obtained from the observed LOS velocities and the component perpendicular to the LOS derived from the ionospheric potential model (Ruohoniemi and Baker 1998). As a powerful tool for monitoring the geospace environment, the SuperDARN radar network enables us to examine the global ionospheric convection pattern relevant to the evolution of magnetic flux that couples the interplanetary space and the Earth’s magnetosphere-ionosphere system after magnetic reconnection (Chisham et al. 2007; Lester 2008, 2013).
As described above, a two-cell circulation pattern with the dawn cell in counter-clockwise circulation and the dusk cell in clockwise circulation is usually observed by the SuperDARN on the orientation of southward IMF. This kind of ionospheric convection is driven by the dawn-dusk electric field, which is mapped from the magnetopause and magnetotail into the high-latitude ionosphere along the conducting and equipotential magnetic field lines. By measuring the motion of this ionospheric plasma, it is, therefore, possible to infer a great deal about the magnetospheric processes that are responsible for the convection. Concerning the present complex convection pattern with small reversed sub-cells in the cusp region, both the northward IMF and shock disturbance are responsible for the formation of the ionospheric convection pattern.
Using global geomagnetic field measurements and real event parametric simulation results, Han et al. (2010) revealed that high-latitude magnetopause reconnection was really triggered by the sudden shock compression, and certainly the reconnection rate was enhanced by the shock compression accordingly. Corresponding disturbed reconnection electric fields at a higher latitude magnetopause mapped along the geomagnetic field lines into the polar ionosphere, driving the small sub-cells circulation nested in the cusp. Although the IMF component was dominated positive before the shock arrival, the ionospheric convection was relatively stable as well as displayed in Fig. 7. Therefore, the presence of a four convection cells pattern in this event is a strong consistent evidence for the occurrence of lobe reconnection along the high-latitude magnetopause tailward of the cusp after the shock arrival (Crooker 1992; Hu et al. 2006; Lu et al. 2011). In other words, the intensified and equatorward-moving discrete auroral filaments that we observe are the typical optical feature that can be attributed to lobe reconnection occurring along the high-latitude magnetopause during shock compression. Furthermore, the polar cap size does not change noticeably during the shock compression induced from the stable poleward boundary of discrete red emission band, which is another evidence of lobe reconnection (Cowley and Lockwood 1992; Milan et al. 2003). Hubert et al. (2006) also obtained that the accumulated open flux is closed by intense magnetotail reconnection under strong shock compression, but little flux was closed by these shocks under mostly northward IMF lasting several hours.
A favorable conjunction of the all-sky imager and SuperDARN radar allows us to study the simultaneous aurora and ionospheric response to an interplanetary shock occurring under northward IMF conditions. The specific signature of the diffuse aurora appearing as a uniform structure in the lower latitude region responding to the shock compression is an immediate poleward motion just after the SI onset. Nevertheless, the discrete aurora is characterized by a gradual increase of the auroral intensity and a widening of the auroral oval as the magnetosphere is disturbed.
From this special event study, we conclude that: (1 More accurate response time of diffuse aurora to sudden shock impact was confined within 10 s; (2 Loss cone instability triggered by sudden shock compression and subsequent enhanced wave-particle interaction were responsible for the occurrence and associated evolution of diffuse aurora; (3 By coordinated SuperDARN radar measurements, it is confirmed that the intensification and the equatorward motion of filaments of the discrete aurora was caused by lobe reconnection occurring along at a high latitude along the magnetopause during the shock compression; (4 Based on high temporal and spatial resolution ground-based imaging data, it is ascertained that the shock-induced aurora is a diffuse-type emission at the lower latitudes of the dayside auroral oval and discrete aurora on the oval with an overlap of the two types of aurora across a few degrees of latitude.
The authors are grateful to SuperDARN PIs for sharing their data. SuperDARN is a collection of radars funded by national scientific funding agencies of Australia, Canada, China, France, Japan, South Africa, the UK, and the USA. We would like to thank Xiangcai Chen who implemented optical aurora mapping to the MLAT-MLT coordinate system developed from UiO techniques and gave a very helpful discussion. The ACE IMF and solar wind data were provided by CDAWeb service (http://cdaweb.gsfc.nasa.gov). The IMAGE chain magnetometer data were downloaded from the following website: www.ava.fmi.fi/image/, and lower latitude geomagnetic data were obtained from WDC at Kyoto and INTERMAGNET. This work is supported by the National Natural Science Foundation of China (41431072, 41304149, and 41374161), the Polar Environment Comprehensive Investigation and Assessment Programs (CHINARE 2014-02-03), the International Collaboration Supporting Project, Chinese Arctic and Antarctic Administration (IC201303), the Pudong development of scientific and technology program (PKC2013-207), and the project is supported by the Specialized Research Fund for State Key Laboratories. Zhongshan HF radar as a member of SuperDARN is funded by Chinese Meridian Project.
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