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Simultaneous ground-based optical and SuperDARN observations of the shock aurora at MLT noon

  • Jianjun Liu1, 2Email author,
  • Hongqiao Hu1,
  • Desheng Han1,
  • Huigen Yang1 and
  • Mark Lester3
Earth, Planets and Space201567:120

https://doi.org/10.1186/s40623-015-0291-2

Received: 21 December 2014

Accepted: 8 July 2015

Published: 29 July 2015

Abstract

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.

Keywords

Interplanetary shockSudden impulseOptical auroraSuperDARNSunward flow

Background

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.

Methods

Instrumentation

In this paper, we utilize ground-based magnetometers data from IMAGE chain in Scandinavia for investigating the geomagnetic field response in the polar region (shown in Fig. 1 by solid dot), INTERMAGNET Addis Ababa and WDC Kakioka magnetometers were used for monitoring simultaneous low-latitude geomagnetic measurements. Ground-based optical auroral data obtained from YRS at Ny-Ålesund (NYA) in Svalbard, which is situated near 76° corrected magnetic latitude on 7 January 2005. The optical system at YRS includes three identical ASIs (wavelength of 427.8, 557.7, and 630.0 nm, respectively) and consists of a 180° FOV fish-eye lens, a relay lens, an automated filter lens, a focus lens, and air-cooled CCD camera with a resolution set at 512 × 512 pixels for monitoring auroral two-dimensional behavior (Hu et al. 2009). In this paper, we use the red (OI, 630.0 nm) and green (OI, 557.7 nm) auroral emissions monitored by the ASIs to inspect the visible aurora fine structure response to prompt shock compression. The shaded circle in Fig. 1 shows the FOV of the ASI at YRS projected to roughly a 200-km altitude. During the whole winter of 2005, the exposure and readout times of the all-sky cameras were set at 7 and 3 s, respectively. Thus, the time resolution of tahe optical aurora data is 10 s. Based on its superior geomagnetic location in the polar cusp region and multi-wavelength optical imaging instruments, YRS is an ideal auroral observatory for continuously monitoring dayside auroral emissions during the whole winter in the Northern Hemisphere, and can provide plentiful source data for auroral investigations since its initial operation in late 2003 (Hu et al. 2009; Hu et al. 2010; Zhang et al. 2010; Hu et al. 2012).
Figure 1
Fig. 1

A magnetic latitude-magnetic local time (MLAT-MLT) projection of the Northern Hemisphere at 09:22 UT on 7 January 2005. Coverage of the instrumentation in polar region used in the study; the shaded circle shows the FOV of the ASI at YRS, the FOV of the SuperDARN CUTLASS Finland HF radar, its individual beams referred to in the text are bounded by solid lines and numbered approximately, and the four solid dots give the locations of the IMAGE chain magnetometers aligned with YRS. The IP shock plane roughly indicating the impingement is shown at the top of the figure

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.

Observations

Solar wind and geomagnetic field response

As shown in Fig. 2, an interplanetary fast-moving forward shock was observed at ~08:40 UT when the ACE spacecraft was at (229, −40, and 23 RE). At the shock, the solar wind dynamic pressure increased suddenly from ~1.8 to 3.6 nPa due mainly to a clear increase in proton density and solar wind speed. Sibeck (1990) showed that δp/p, not δp, is the main factor for deciding the effect of the transient magnetospheric responses to sudden solar wind dynamic pressure variations. For this event, the amplitude of the solar wind dynamic pressure pulse (δp/p) is about 1.0, which is large dramatically as defined by Sibeck (1990), so we can expect clear compressional effects in the magnetosphere-ionosphere system and geomagnetic field. The IMF magnitude increased from 5.2 to 7.2 nT at the shock. The IMF Bz component was positive (northward) in the shock upstream, and experienced brief excursion to negative (southward) just downstream of the shock, so it can be expected that the magnetosphere was not much loaded with open magnetic flux. The IMF By was weakly negative near zero upstream and turned positive downstream of the shock. For this shock, magnetic coplanarity (MC), velocity coplanarity (VC), three mixed methods (MX1, MX2, MX3) (Schwartz 1998), and the Rankine-Hugoniot method were used to determine the shock normal, shock speed, and mach number (Berdichevsky et al. 2000). The calculated shock normal vector, which strongly influences the nature of the shock, is (−0.873, −0.445, 0.200) in GSM coordinates , and the shock Mach number is 1.62 with a shock speed of 522.5 km/s along the normal direction (Wang et al. 2010). It is investigated that most of the shock orientation are in the range 130–170°; an angle of 180° indicates the shock is antiparallel to the Sun-Earth line and thus hits the magnetosphere head-on (Wang et al. 2009). This shock front is estimated to hit the magnetopause at a local time of ~1030 (shown in Fig. 1), and the auroral initial brightening was expected to occur near local noon. The bottom panel of Fig. 2 shows the Sym-H index used to determine the responses of the geomagnetic field in the low-latitude region to the IP shock compression and related dynamic process. Sudden featured increase in the Sym-H index at ~09:22 UT from a low stable value indicates that a geomagnetic sudden impulse (SI) was triggered by the shock compression. Indeed, such SI signature was shown to be a good indicator of IP shock arrival to the magnetosphere (Wang et al. 2010).
Figure 2
Fig. 2

ACE solar wind data and geomagnetic Sym-H index for the interval 06:00-12:00 UT on 7 January 2005. From top to bottom they are: IMF Bz in GSM coordinates, Bx and By components, Solar wind proton density (Nsw), Velocity of the solar wind X component, Solar wind dynamic pressure (Pdyn), Geomagnetic Sym-H index. Two vertical dashed lines indicate the shock time (08:40 UT) recorded by ACE and the arrival time (09:22 UT) of the shock to the magnetosphere

Figure 3 shows the geomagnetic field observations of the SI by fluxgate magnetometers distributed from low latitude to the polar region in the Northern Hemisphere. Geographical locations of these four polar observatories were indicated by solid black dots in Fig. 1. Besides Kakioka, which provides one second resolution data in East Asia, the other five magnetic observatories are roughly aligned along the same geographical meridian where YRS is located. It is indicated that the geomagnetic field was relatively stable before the shock arrival at 09:22 UT marked by the vertical dashed line in Fig. 3. The geomagnetic field variation associated with the SI in low-latitude stations such as Addis Ababa and Kakioka presents simple monotonic enhancement of its northward components. This apparent increase of the geomagnetic field intensity in lower latitude region was produced mainly by enhanced eastward electric currents flowing on the magnetopause and a propagating compressional wave front associated with shock compression (Araki 1994). It should be noted that the simultaneous geomagnetic field response in the polar region was essentially different from those observed at lower latitude, which first showed a preliminary negative impulse followed by a main impulse. Previous research revealed negative impulse was caused by the instant dusk-to-dawn electric field, which was transmitted to the polar ionosphere from the compressional wave front propagating in the dayside magnetosphere (Araki 1994; Han et al. 2010). Subsequent larger positive impulse in the main phase of the SI was associated with the enhanced large-scale dawn-to-dusk convection electric field. In general, the shock impact triggered significant and direct electromagnetic environmental change in geospace.
Figure 3
Fig. 3

Geomagnetic field observations measured by magnetometers from low latitude to polar region in the Northern Hemisphere between 09:00 and 10:00 UT. The vertical dashed line indicates the onset time of the SI

Optical auroral data

Just at the moment of the interplanetary shock impacting to the terrestrial magnetosphere, YRS in the northern polar region located at almost magnetic local noon (~1210 MLT) as well under the ionospheric footprint of the magnetospheric cusp region (Hu et al. 2009; Zhang et al. 2010). This superior geomagnetic position right beneath the dayside auroral oval with high quality optical auroral data provides a unique opportunity to study the dayside auroral fine structure in the context of the dynamic disturbed magnetosphere-ionosphere coupled system. Figure 4 shows the 30 s interval’s auroral image sequence in green line emissions performed at YRS during 09:20:00–09:30:30 UT (optical wavelength centered at 557.7 nm). Frames at 09:20:00 and 09:21:00 UT shortly before the shock arrival illustrate the in-situ background auroral emission in the cusp region. The following 18 frames with 30-s time resolution show the aurora during the shock compression, identifying its detailed bright and motional evolution. The capture time is written at the top of each frame. The red dashed line between 100 and 110E° meridian line indicates the magnetic local noon, and NYA at Svalbard was marked at the center of each frame.
Figure 4
Fig. 4

Green line emissions of the shock aurora at 557.7 nm observed at YRS station on 7 January 2005. Auroral sequence images were shown with cadence of 30 s during 09:22:00–09:30:30 UT. A MLAT-MLT coordinate grid was plotted in each frame. SI onset is marked by the black arrow in the first row

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.

Figure 5 presents the red auroral line emissions at 630.0 nm in the same format as Fig. 4. Before the SI onset marked by the downward black arrow, the auroral images display the discrete type aurora in dayside corona elongated in the east-west direction at near the northernmost portion of the FOV, which is the luminous band and stable structured auroral emission intersecting with minor beams of auroral electrons at the edge of the FOV. Compared with sudden brightening and expanding of diffuse aurora to the shock impact shown in Fig. 4, dayside discrete corona’s responding is not so quick and obvious at the preliminary stage of the SI. Initial typical enhancement of auroral luminosity can be seen mainly in the northeast part of the emission band. The gradual variation of the dayside discrete aurora was indicated by the oblique black arrow in the third frame of Fig. 5. Actually, the dayside corona of aurora remained a relatively steady narrow luminous band shape during the first two minutes after the SI onset, apparent variation began at 09:23:50 UT with an auroral form gradually moving equatorward (i.e., sunward) from the middle portion of the band (shown by the black arrow) and prominent increased intensity within the FOV. That is to say, two minutes after the SI onset, the discrete red aurora was intensified noticeably in the ASI images, which leads to a broadening of the latitudinal width of the bright band. The gradual intensity increase and sunward expansion of the lower latitude boundary of the discrete aurora are significantly different from the abrupt reaction and fast poleward motion of the diffuse aurora at 557.7 nm described above. On the other hand, the brightened structure was also characterized by eastward propagation, especially for the central beam structures of the emission band, meaning the discrete aurora also moved toward the afternoon sector along the auroral oval following its first brightening in the midday sector.
Figure 5
Fig. 5

Same format with Fig. 4, but for red line emissions are at 630.0 nm

The auroral keogram for the green and red lines, which were created by extracting the pixel column along the geomagnetic north-south meridian from individual all-sky images with 10-s resolution obtained by ASIs at YRS and putting these columns side by side are shown in Fig. 6. The horizontal and vertical axes are universal time and zenith angle, respectively. Figure 6a shows that the diffuse aurora in the southern sky responds promptly to the shock sudden compression as occurring almost simultaneously with the SI onset at 09:22 UT marked by the red dashed vertical line. The diffuse aurora, manifesting as a uniform structure, featured instant brightening and subsequent poleward motion marked by the white arrow in Fig. 6a. It is shown that this type of aurora soared up a higher latitude within an extremely short time period. By contrast, the dayside band shaped discrete aurora in the higher latitude region shown in Fig. 6b presented an equatorward moving of its lower latitude boundary, which accordingly results in a broadening of the auroral oval in the local noon sector. In particular, the poleward boundary of the dayside corona of aurora was almost stable before and after the SI. Overall, the discrete auroral intensity increased during magnetospheric compression, especially in the lower latitude portion close to right zenith of the ASI.
Figure 6
Fig. 6

Auroral keograms in 557.7nm and 630.0nm wavelengths from YRS are presented in two panels between 09:00 and 10:00 UT. The left vertical axis gives the zenith angle from -90º(equatorward) to 90º(poleward), and corresponding magnetic latitude was shown in right vertical axis. The red vertical dashed line indicates the SI onset time

SuperDARN radar observation

The SuperDARN CUTLASS Finland radar at Hankasalmi (63.32° N, 26.61° E), which has good scanning coverage of the ASIs at YRS as shown in Fig. 1, observed the ionospheric plasma irregularities and associated plasma flow during the shock compression in the midday sector. Figure 7 presents a sequence of three scans from the radar measurements before and after the SI showing, from top to bottom, the backscatter power, the line-of-sight (LOS) velocity and the spectral width. The radar data of the backscatter power are characterized by a loose band of power echoes elongated approximately at geomagnetic latitudes of ~78°–83° before the shock arrival; some power echoes on the near range gates were calculated as mainly ground backscatter echoes marked by shaded squares in LOS data. After the SI onset at 09:22:00 UT, the backscatter power was obviously enhanced and the echo band was broadened due to more detected wide echoes, especially in the eastern portion of the radar FOV, which roughly corresponds to the discrete auroral bright spot situated longitudes range from ~120 to ~150 E° at 09:23:00 UT in Fig. 5. It is worth noting that the sharp equatorward edge of the backscatter band moved southward, namely closer to the north of Svalbard. Two minutes later (09:25:00 UT), the intensified echo power in the band spread azimuthally aligned in the east-west direction. Compared with the power echo data before 09:22:00 UT, the typical eastward plasma irregularities were impressive after the SI onset. Milan et al. (1997) did backscatter occurrence statistics from the CUTLASS radars, they determined that ionospheric backscatter is observed at far ranges during the local day in winter months. Concerning to the present event, the regional distribution of ionospheric backscatter echoes in the cusp region were approximately correlated with the occurrence region of the dayside discrete aurora shown both in Figs. 5 and 6.
Figure 7
Fig. 7

CUTLASS Finland radar echo power, LOS velocity and spectral width at 09:20:00, 09:23:00 and 09:25:00 UT on 7 January 2005 were shown in MLAT-MLT coordinates. In each plot, noon is to the top and dusk to the left as marked in the first plot. The concentric dashed circles represent 10° increments of magnetic latitude, marked at 60°, 70° and 80°

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.

Figure 8 presents radar magnetic latitude time plots of backscatter echo power and LOS velocity parameters between 09:00 and 10:00 UT by beams 6 and 11, respectively. Before the IP shock arrival to the Earth space, ionospheric backscatter echoes were mainly corresponding to a narrow latitudinal region between ~78° and ~80° MLAT, while the LOS velocity measurements show weak sunward (antisunward) flow in the western (eastern) portion. Both beam’s observation measured dramatically increased backscatter echoes and power after the SI onset illustrated by the vertical dashed red line. The interesting feature after the shock initial compression is the sudden appearance of ionospheric plasma irregularities from the higher latitude ionosphere, especially typical in observations by beam 11. In addition, the ionospheric plasma convection in the polar cap region presents a high speed flow toward the radar site (circled by the black ellipse), namely sunward flow. This signature of sunward ionospheric convection in the polar cap region is not very common as it departs from the usual dominant flow pattern presenting two convection cells forming an antisunward flow in the polar cap and a return flow at lower latitude.
Figure 8
Fig. 8

Backscatter power and LOS velocity plots for beams 6 and 11 of the SuperDARN CUTLASS Finland HF radar. The red dashed vertical line indicates the onset time of the SI, and the black circular mark the sunward flow

Results and discussion

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).

Figure 9 displays the large-scale flow pattern in the Northern Hemisphere between 09:24 and 09:26 UT, which can be used as a good indicator of the temporal evolution of the magnetic reconnection and topology. Data are plotted in the altitude-adjusted corrected geomagnetic (AACGM) coordinates from 60° to 90°MLAT with noon on the top and dawn on the right as viewed above the North Pole such that the Sun is on the top (Baker and Wing 1989). Note that the impressive signature of the convection map consists of four convection cells, with two localized reversed convection cells formed in the dayside polar cap region nested between two normal convection cells at lower latitudes on the dawnside and duskside, respectively. It is clear that the global convection map shows prominent and exact sunward plasma flows in the local noon sector after the shock arrival.
Figure 9
Fig. 9

Two-dimensional ionospheric convection pattern derived from the SuperDARN radars at 09:24–09:26 UT

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.

Conclusions

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.

Declarations

Acknowledgements

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.

Authors’ Affiliations

(1)
SOA Key Laboratory for Polar Science, Polar Research Institute of China, Shanghai, China
(2)
State Key Laboratory of Space Weather, Chinese Academy of Science, Beijing, China
(3)
Department of Physics and Astronomy, University of Leicester, Leicester, UK

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© Liu et al. 2015

This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly credited.

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