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Substorm and pseudo-substorm Pi2 pulsations observed during the interval of quasi-periodic magnetotail flow bursts: A case study
© The Society of Geomagnetism and Earth, Planetary and Space Sciences (SGEPSS); The Seismological Society of Japan; The Volcanological Society of Japan; The Geodetic Society of Japan; The Japanese Society for Planetary Sciences; TERRAPUB 2010
Received: 6 July 2009
Accepted: 10 December 2009
Published: 17 June 2010
We studied the relationship between midtail flow bursts observed by the Geotail spacecraft and eight Pi2 pulsations near midnight observed at low-latitude Kakioka (KAK, L = 1.26) and high-latitude Tixie (TIX, L = 5.9) stations on 26 October (day 299) 1997, 1100–1600 UT. The Pi2 pulsations at KAK have a great similarity with those at TIX with an out of phase signature. Three of the Pi2 bursts were associated with substorm onsets/intensifications and other five events were associated with pseudo-substorm onsets. The pseudo-substorm Pi2 pulsations exhibited longitudinal phase variations similar to substorm-related Pi2 pulsations. From this observation we suggest that pseudo-substorm associated current system is morphologically the same as substorm current wedge. The substorm Pi2s are enhanced at higher frequency band (∼ 15–20 mHz) than the frequency band (∼6–15 mHz) of pseudo-substorm Pi2s. We do not attribute these frequency variations to the change of the plasmapause distance, which is favored in the plasmaspheric resonance model. During the five-hour interval, Geotail observed quasi-periodic high-speed flow bursts (perpendicular flow velocity V⊥x > 300 km/s) preceding the low-latitude Pi2 pulsations by ∼35–150 s. It is found that there is no obvious relationship between the speed of the earthward flow burst events and the power of the Pi2 events. This means that enhanced flow speed is not a main factor in controlling a Pi2 power. The waveform and period of the Pi2 pulsations are different from those of the flow bursts except for one event, which was previously reported as BBF-driven Pi2.
Pi2 magnetic pulsations are low-frequency (period = 40–150 s) oscillations of the geomagnetic field (e.g., Saito, 1969). They are usually excited at the onset of a geomagnetic substorm and last for a few cycles. Currently, plasmaspheric cavity mode resonance is the most popular source mechanism for Pi2 pulsations observed at low to mid latitudes. A number of statistical and case studies using ground-based observations or simultaneous ground and satellite observations have reported that low-latitude Pi2 pulsations are consistent with plasmaspheric resonances (e.g., Takahashi et al., 1995, 2001, 2003; Kim et al., 2001, 2005a; Nosé et al., 2003; Han et al., 2004).
The plasmaspheric resonance is not the only explanation given for low-latitude Pi2 pulsations. Recently, it has been proposed that low-latitude Pi2 pulsation can be generated by time-modulated plasma bulk flows in the near-Earth magnetotail. Kepko and Kivelson (1999) and Kepko et al. (2001) showed several examples of low-latitude Pi2 waves and midtail flow oscillations that have nearly identical waveforms. The authors suggested that the intermittent compressional waves generated by flow-braking (Shiokawa et al., 1998) directly drive low-latitude Pi2 pulsations. That is, midtail flow bursts are directly and causally linked with low-latitude Pi2 pulsations. Several case studies suggested that the flow-driven mechanism plays a role in determining the spatial and spectral properties of Pi2 pulsations (Osaki et al., 1998; Kim et al., 2005b; Cao et al., 2008).
Other studies that compared midtail plasma flows and Pi2 pulsations, however, found little evidence of the latter being driven cycle-by-cycle by the former. Yamaguchi et al. (2002) surveyed coordinated observations of a Pi2 onset on the ground, at geosynchronous altitude, and in the near-Earth plasma sheet with a strict requirement for the spatial alignment of observation points. The authors found that the waveforms of the low-latitude Pi2 pulsations are quite similar to the magnetic pulsations at geosynchronous orbit, but that the earthward flow variations in the plasma sheet are not similar to the Pi2 pulsations. Murphy et al. (2006) compared enhanced earthward flows and ground Pi2 pulsations from high to low latitudes. They found no direct link between the period in the flow bursts and the period of Pi2 waves. These observations suggest that flow bursts are not the cause of Pi2 pulsations.
List of ground magnetometer stations.
Since Pi2 pulsations are commonly observed at the onset of a magnetospheric substorm, Pi2 pulsations have been considered as one of substorm indicators. However, it has been reported that Pi2 pulsations sometimes occur under extremely quiet solar wind condition and magnetospheric condition (e.g., Sutcliffe, 1998; Lyons et al., 1999; Sutcliffe and Lyons, 2002; Kim et al., 2005b). That is, Pi2s can occur during the absence of substorm. The question thus arises as to the origin of such Pi2s and whether they have spatial variations similar to substorm-associated Pi2s.
In this study we show eight well-defined low-latitude Pi2 pulsations. Three of the Pi2 bursts were associated with substorm onsets/intensifications and other five events were observed without a significant substorm signature on the ground and in space. They occurred during an interval of quasi-periodic or bursty midtail flows detected by Geotail. Since the flow bursts preceded the Pi2s by ∼35–150 s, we examine if the low-latitude Pi2 pulsations have a causal relationship with the flow bursts.
2. Data Sets
We studied Pi2 pulsations using high-latitude Kotelny (KTN) and Tixie (TIX) and low-latitude Kakioka (KAK) magnetometer data. The low-latitude magnetometer data from the 210 MM magnetic network are also used to examine the spectral analysis (Yumoto et al., 1996). The geographic and corrected geomagnetic coordinates (CGM) for the ground stations are listed in Table 1. Magnetic field measurements at KTN, TIX, and KAK are made at 1-s intervals, but we reduced the time resolution to 6 s by running an average to discuss the properties of Pi2 pulsations. The auroral electrojet indices AL and AU, provided in 1-min resolution, are used to illustrate geomagnetic activity and to find the onset of substorms.
The Pi2 events reported in this study occurred during a 5-hour interval, 1100–1600 UT on 26 October 1997. We identified eight nightside Pi2 events at KAK. Five of the Pi2 events were accompanied by quasi-periodic flow bursts observed by Geotail in the magnetotail. We examine in detail the relationship between the flow bursts and the ground Pi2 pulsations.
3.1 Solar wind observations
3.2 Overview of the low-latitude Pi2 events
During the interval 1100–1400 UT, the magnitude of AU was less than 50 nT. In the 3-hour interval 1100–1400 UT during which Pi2 events A–E occurred, the AL index maintained a small magnitude (<50 nT) and there is no sudden decrease of AL. These low geomagnetic activities are associated with the northward IMF interval. At KAK positive H bay was absent for events A–E, implying that a substorm current wedge was not formed (Clauer and McPherron, 1974). Pi2 pulsations without substorm signatures have been reported by previous studies (Takahashi et al., 1997; Sutcliffe and Lyons, 2002; Kim et al., 2005b).
Events F–H were accompanied by AL decrease and a baseline change in H and/or D, implying that the Pi2 pulsations are substorm-associated phenomena. Events F and G show typical low-latitude Pi2 signatures, that is, Pi2 pulsations were superposed on the positive bay. At the onsets of events F and G, KAK was near midnight and observed a large positive increase in H and a small positive increase in D. This implies that KAK was located near the center of the substorm current wedge (Clauer and McPherron, 1974).
The power of the Pi2 events differs from one event to another. The substorm-associated Pi2s (events F and G) have large power. By contrast, the intensity of events A–E during the interval of quiet geomagnetic conditions is clearly lower. This would be related to the source intensity. Takahashi et al. (2002) reported that large (small) Pi2 amplitude is associated with strong (weak) auroral power. Thus, the modulated Pi2 power in our study may be due to the event-to-event variation of auroral activity.
3.3 Observations of particle flux at geosynchronous orbit
At geosynchronous orbit there were no proton injections for events A–E and event H. We note that 1994–080 was at a good location (∼ 18–22 LT) for detecting protons drifting westward from the injection source region. Thus, the absence of injections at 1994-080 indicates that injection did not occur at geosynchronous orbit. The absence of injection at geosynchronous satellite does not mean that there was no injection in the near-Earth magnetotail. As shown in Fig. 2(a), there were small AL variations for events A-Eso we would expect that injections occurred beyond geosynchronous orbit. From these geosynchronous and AL observations, we suggest that events A–E were associated with pseudo-substorm onsets (Koskinen et al., 1993; Ohtani et al., 1993; Takahashi et al., 1997).
Events F and G were accompanied by proton injections that appear in all four energy channels. The proton injections were associated with substorm onsets as shown with an AL decrease and a positive bay at KAK. There was a proton injection at ∼1540 UT when the AL index showed a sudden decrease. These phenomena are commonly observed at the onset of a substorm. However, there was no low-latitude Pi2 pulsation at ∼1540 UT. This indicates that low-latitude Pi2 pulsations are not always accompanied by AL decrease and particle injection. 3.4 Observations at high-latitude ground stations
A clear onset of a negative H perturbation with a dramatic change (A H ∼−700 nT in less than 5 min) was observed at KTN at ∼1454 UT, indicated by the second vertical dashed line, when event G and positive H bay were observed at KAK. At this onset time, the perturbation in the Z component was positive at KTN and negative at TIX. These Z variations clearly indicate that the westward electrojet current was formed between TIX and KTN. At the onset of ∼ 1454 UT, the H component at TIX exhibited a positive perturbation. This positive perturbation could be explained by the field-aligned current or distorted electrojet (Kisabeth and Rostoker, 1973). During event G, the H component at TIX decreased ∼−100 nT compared to the baseline before 1435 UT. This amplitude is smaller than that at KTN. This result indicates that the westward electrojet intensified near KTN, poleward of TIX.
In event A, KAK data exhibits approximately three cycles of oscillation, but TIX and KTN data show different variations. We note that a sinusoidal perturbation with a period much longer than the Pi2 period, starting at the onset of event A, was observed at TIX and KTN (see Figs. 6(a) and 6(b)). The Pi2 oscillation looks like to be superposed on the slow field variations. In fact, we can find that there are field perturbations at TIX, which correspond to the KAK Pi2 peaks, following the vertical dashed lines. TIX H oscillates out of phase with KAK H. The perturbations at KTN H are similar to those at TIX during event A. Their amplitudes are comparable to each other.
For events B–G, TIX H and KAK H recorded pulsations with nearly identical waveform and period with out-of-phase delay. This implies that the low-latitude and high-altitude Pi2 pulsations in our study are excited by a common source and the same generation mechanism. KTN H also shows out-of-phase oscillations with KAK H for events B– F, but the oscillations at KTN are more irregular and smaller in amplitude than at TIX. Unlike at TIX, KTN had no magnetic field perturbations corresponding to the KAK Pi2 peaks (marked by solid circles on the KTN H trace) for events C and D.
There were pulsation activities at KTN and TIX for event H, but they had no clear cycle-by-cycle correspondence to Pi2 pulsation at KAK. This may be due to the large and slow magnetic field disturbances at TIX and KTN. At auroral zone highly irregular magnetic field disturbances are commonly observed. They are associated with the development of the auroral electrojet. These perturbations are much slower than Pi2 oscillation and much larger in amplitude. Pi2s could be easily masked by such background disturbances.
3.5 Geotail observations in the magnetotail
3.6 A comparison of Pi2 waveform and quasi-periodic earthward BBFs
Geotail observed high-speed V⊥x bursty flows for the interval of event G when the satellite was at GSM (x, y) = (−15.39, −3.45) RE. Their peaks occurred at 14:54:40, 14:55:41, 14:56:30, and 15:00:21 UT, respectively. If the bursty flows are shifted to the right by 35 s, this time shift produces a nearly perfect match of the first three and seventh KAK H peaks. However, there are no flow bursts corresponding to the fourth, fifth and sixth peaks of the Pi2 pulsation at KAK.
During event E, the KAK H peak at 13:40:34 UT matches the earthward V⊥x peak at 13:39:19 UT if time is shifted 75 s. From 1341 to 1348 UT, V⊥x oscillated with a period much shorter than event E. Such a short-period oscillation cannot be identified in the H component at KAK. For event D, although there are flow bursts that match the Pi2 peaks with 148-s time shift, we cannot find matching for the entire Pi2 wave packet.
It has been recently suggested that low-latitude Pi2 pulsation can be directly driven by periodic earthward flow bursts in the middle magnetotail. Kepko and Kivelson (1999) and Kepko et al. (2001) reported several examples of low-latitude Pi2 pulsations and midtail earthward flow bursts that have nearly identical waveforms. The midtail bursts started 60–180 s earlier than the low-latitude Pi2 pulsations. Thus, the authors suggested that the flow bursts directly drive the Pi2 pulsations and that the Pi2s have a causal relationship with flow burst events.
We observed eight Pi2 events at KAK on 26 October 1997, 1100–1600 UT. Five of them had no significant sub-storm signatures (called pseudo-substorm Pi2s) as shown in Figs. 2 and 5, and other three events were associated with substorm onsets/intensifications. Since there were no bay signatures for the pseudo-substorm Pi2s, they did not originate from an oscillation of currents flowing on the substorm current wedge.
As shown in Fig. 4, the longitudinal polarization pattern of the pseudo-substorm Pi2s is the same as that of substorm-associated Pi2. This implies that the Pi2-associated current system for the pseudo-substorm onset is morphologically the same as substorm current wedge. We suggest that the oscillations of field-aligned current on the Pi2 current wedge produce ground perturbations on the east-west component at KAK (see Fig. 3), which explain the longitudinal variation of polarization axis (Lester et al., 1983).
The substorm-associated Pi2s (events F–H) are enhanced at higher frequency band (∼ 15–20 mHz) than the frequency band (∼6–15 mHz) of pseudo-substorm Pi2s (events A– E). If such frequency increase from ∼6–15 mHz to ∼15–20 mHz is caused by the plasmapause distance decrease, it is expected that the plasmapause moves inward to L ≈ 3.5 from L ≈ 4.5 (Gallagher et al., 1995; Takahashi et al., 2003). According to recent studies (Goldstein and Sandel, 2005, and references therein), inward motion of the nightside plasmapause occurs ∼20–30 min after the arrival of southward IMF at the dayside magnetopause. We expect that the inward motion of the plasmapause begins at ∼1400 UT. Then, the plasmapause erosion rate is 2.0 L per hour of UT. This erosion rate is much larger than during the interval reported by Spasojević et al. (2003), which has similar geomagnetic and IMF conditions to the interval in our study. Therefore, the Pi2 frequencies in our study are not controlled by the plasmapause distance. We suggest that the Pi2s in our study may be associated with transient responses to the variations in the magnetotail.
During the Pi2 events we observed quasi-periodic earthward flow bursts preceding low-latitude Pi2 pulsations by ∼35–150 s. Kepko et al. (2001) suggested that the high-latitude Pi2 pulsations can be generated by time-modulated BBFs. According to the BBF-associated Pi2 model, dawn-ward directed current perpendicular to the magnetic field is generated by the inertia effect as the time-modulated earthward BBFs are decelerated or braked in the tail/dipolar transition region. The perpendicular current is diverted into the field-aligned currents that flow on a wedge-shaped circuit connected to the ionosphere. The current system decays as the flow disappears but it intensifies again when the next flow burst arrives. As mentioned above, pseudo-substorm Pi2s occurred without background field change, i.e., without the substorm current wedge (see Figs. 2 and 6). Thus, the pseudo-substorm Pi2s could be explained by the time-varying braking inertial current. However, the time-modulated BBF model cannot provide a complete explanation of our observation because we do not find any systematic correlation between Pi2 power and the flow-burst intensity.
In the BBF-driven Pi2 events presented by Kepko et al. (2001, 2004), the earthward flow bursts preceded the low/mid-latitude Pi2 events by 60–180 s. This time delay is comparable to that in our study except for event G, which had a 35-s time delay. Note that Geotail was at GSM (x, y, z) ≈ (−15.4, −3.4, 0.1) RE for event G. If flow deceleration or braking at geocentric distance of ∼ 10–15 RE (Shiokawa et al., 1998) plays a major role in exciting the Pi2 pulsations, the 35-s time delay is too short for the travel time of an Alfvén wave from the braking region to the ionosphere. Furthermore, we observed a small Pi2 events just before event G (see Fig. 13) preceding a single earthward flow burst by ∼10 s. If event G and the small Pi2 event are associated with the earthward flow bursts, the Pi2 current system may be formed before the flow bursts are observed at Geotail. This leads us to suggest that field-aligned current producing the Pi2 perturbations occurs at a radial distance greater than the flow braking region (see figure 19 in Birn et al., 2004). To confirm this suggestion, we need to examine the spatial characteristics of the earthward flow burst from the tail reconnection region and the flow braking region using multipoint measurements.
We showed that the pseudo-substorm Pi2 power is much smaller than the substorm-associated Pi2 power by a factor of ∼ 10–100. This can be explained if the substorm-associated current is larger than the inertial current by a factor of 10–100 (Birn et al., 1999). It should be noted that the peak speed and duration of the flow burst corresponding to pseudo-substorm events (events D and E) are comparable to those of substorm-associated Pi2 (event G). This implies that the BBFs observed at Geotail may not be a main parameter to directly control substorm and/or pseudo-substorm activities.
The temporal variations of the flow bursts observed at Geotail are compared with Pi2 pulsations. It is found that the waveform and/or period of the low-latitude Pi2s are significantly different from those of the flow bursts. From these observations we cannot conclude that the KAK Pi2s in our study are directly driven by the midtail earthward flow bursts observed at Geotail.
List of the flow burst events with V⊥x > 300 km/s.
B x nT
B y nT
B z nT
B xy a nT
B z /B xy
Table 2 summarizes the characteristics of the Geotail data for thirteen flow burst events, identified in Fig. 16. B xy , indicating , is less than 15 nT for all of the flow burst events, and for twelve events out of thirteen events B z /B xy is larger than 0.5. A total of thirteen events were found in the region of β i > 0.5. From these characteristics of the flow bursts, we suggest that the spacecraft was located in the central plasma sheet whenever the high-speed flow bursts were detected (Baumjohann et al., 1990; Nagai et al., 1998). In the central plasma sheet, the flow bursts events (V⊥x) are responsible for the earthward transport of plasmas and magnetic flux. The ion distribution function of the plasma flow with respect to the ambient magnetic field in the plasma sheet or plasma sheet boundary layer can be found in the study of Nagai et al. (1998).
From the magnetic field B x and B z variations in Fig. 16, we can identify that Geotail transiently entered the central plasma sheet region because of plasma sheet oscillations. Such plasma sheet oscillations have been observed near substorm onset (e.g., Bauer et al., 1995). If the flow bursts in the central plasma sheet play a dominant role in exciting low-latitude Pi2s, it is not easy to find a good one-to-one correspondence between the flow bursts and Pi2s with a single-point observation in the magnetotail because the magnetotail is highly fluctuating.
We have studied the Pi2 pulsations observed at high and low latitudes during the interval of quasi-periodic earthward flow bursts on October 26, 1997. We showed that some of the Pi2 events occurred without high-latitude negative bay and geosynchronous proton injection. This indicates that Pi2 pulsations are not always associated with substorm. The pseudo-substorm Pi2s exhibited longitudinal phase variations similar to substorm-related Pi2 pulsations. From these observations, we suggest that the Pi2 current system for the pseudo-substorm Pi2s has the same morphology as the sub-storm current wedge. Unlike in previous studies, our low-latitude Pi2 events have a high degree of similarity with the high-latitude Pi2s. This indicates that the Pi2 pulsations are generated by a common source mechanism. In our study, we favor the field-aligned current oscillation for the source of the Pi2 oscillation rather than the plasmaspheric resonance. According to the BBF-driven Pi2 model, the field-aligned current can be generated by braking of fast flows in the region of strong dipole field. Then, one would expect that the period of flow oscillation should match Pi2’s period. However, the time series examination for the flow burst events at Geotail and Pi2 pulsations at Kakioka did not provide clear evidence for the BBF-driven Pi2 model because Pi2s and flow oscillations do not have nearly identical waveforms. The field-aligned current can also be generated by twisted or sheared magnetic field (Birn et al., 2004), which is caused by earthward flow burst. This indicates that the field-aligned current can be generated by various sources in the magnetotail. Therefore, we need a larger suite of satellites to reveal the full spatial structure of the earthward flow bursts. In the near future, we will attempt to examine the relationship between earthward flow bursts and Pi2 pulsations with multipoint observations, THEMIS and Cluster missions, in the tail.
The ground Kakioka data and the provisional auroral electrojet indices were provided by the Kakioka Magnetic Observatory and the Kyoto University World Data Center C2, respectively. The solar wind and IMF data from Wind were provided by the NASA’s CDAWeb site. Solar-Terrestrial Environment Laboratory, Nagoya University supports construction of the 210 MM magnetometer database. We are grateful to G. D. Reeves for the energetic particle flux data from the Los Alamos National Laboratory geosynchronous spacecraft. This work was supported by WCU program through NRF funded by MEST of Korea (R31-10016). Work at JHU/APL was supported by NASA grants NAG5-13024 and NAG5-13119.
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