Storm sudden commencements (SSCs) occur due to a rapid compression of the Earth's magnetic field. This is generally believed to be caused by interplanetary (IP) shocks, but with exceptions. In this paper we explore possible causes of SSCs other than IP shocks through a statistical study of geomagnetic storms using SYM-H data provided by the World Data Center for Geomagnetism – Kyoto and by applying a superposed epoch analysis to simultaneous solar wind parameters obtained with the Advanced Composition Explorer (ACE) satellite. We select a total of 274 geomagnetic storms with minimum SYM-H of less than –30nT during 1998-2008 and regard them as SSCs if SYM-H increases by more than 10 nT over 10 minutes. Under this criterion, we found 103 geomagnetic storms with both SSC and IP shocks and 28 storms with SSC not associated with IP shocks. Storms in the former group share the property that the strength of the interplanetary magnetic field (IMF), proton density and proton velocity increase together with SYM-H, implying the action of IP shocks. During the storms in the latter group, only the proton density rises with SYM-H. We find that the density increase is associated with either high speed streams (HSSs) or interplanetary coronal mass ejections (ICMEs), and suggest that HSSs and ICMEs may be alternative contributors to SSCs.
Geomagnetic storms are often preceded by a sudden increase of geomagnetic fields, a phenomenon termed storm sudden commencement (SSC). SSC storms occur as the magnetopause is compressed by interplanetary perturbations (Wilken et al. 1982; Tsurutani et al. 1995; Takeuchi et al. 2002). A dominant agent for such perturbations is believed to be interplanetary (IP) shocks. Indeed, many SSCs are accompanied by IP shocks, but with exceptions. Burlaga & Ogilvie (1969) found that all seven SSC events under their study were caused by IP shocks, but reported five IP shocks that were not followed by geomagnetic storms. Chao & Lepping (1974) studied SSCs that occurred during the solar maximum period of 1968-1971 and investigated 48 SSCs with full information on IMF and plasma data, finding that 41 were associated with interplanetary (IP) shocks. Smith et al. (1986) analyzed the data from ISEE 3 satellite and found that during the period of 1978 through 1979, about 75-90% of SSCs were related to IP shocks and 80% of IP shocks were related to SSCs and the others were related to sudden impulses. Wang et al. (2006) performed a statistical study on the SSCs and IP shocks during the period of 1995-2004. About 75% of the SSCs were found to be related to IP shocks. They also investigated effects of speed and direction of IP shocks on SSC rise times and found that the faster IP shocks, the shorter the rising time of the SSC, and that significantly slanted IP shocks may lead to a delay in the rise of the SSC. Russell et al. (1992, 1994) have found that the square root of the dynamic pressure (
We, however, note that not all SSCs are associated with IP shock as already indicated by the afore-mentioned statistical studies. For instance, the finding by Wang et al. (2006) that 75% of SSCs are related to IP shocks implies that there may be alternative drivers for SSCs for the remaining 25%. Correct identification of SSC drivers is important for understanding the dynamics of the Earth's magnetosphere. The relationship between the other geomagnetic activity indices and solar wind parameters has been studied (Oh 2013; Oh & Kim 2013; Kim & Chang 2014a, b). In this paper, we present a statistical study of geomagnetic storms focused on SSCs without IP shocks. We first sort out geomagnetic storms with SSCs that are not accompanied by IP shocks. We then compare their properties with those of SSCs accompanied by IP shocks, as determined using a superposed epoch analysis. From the distinct properties we hope to find clues to the possible cause of SSCs other than IP shocks.
The Disturbance Storm Time (Dst) index is generally used for identifying geomagnetic storms (Sugiura & Wilson 1964). In the present study, however, we use SYM-H (Iyemori 1990), which can also be used as a measure for geomagnetic field change (Wanliss & Showalter 2006). The main reason for choosing SYM-H is that it is given in units of minute while the Dst index is given in units of hour. The higher time cadence of SYM-H is essential for the present study because the increase of geomagnetic fields in SSC occurs in a timescale of tens of minutes. SYM-H used in this study was obtained from World Data Center for Geomagnetism – Kyoto (http://wdc.kugi.kyoto-u.ac.jp/aeasy/index.html).
We also obtain 1-minute average OMNI Web data of IMF magnitude (
Fig. 1 shows solar wind parameters and SYM-H for a geomagnetic storm that exhibits an SSC associated with IP shocks. From the top panel to the bottom panel, we show the interplanetary magnetic field strength,
[Fig. 1.] Physical parameters of the geomagnetic storm on 17 August 2001 showing SSC accompanied by IP shocks. From the top to bottom panel, B, GSM Bz, Vp, Np, and SYM-H are plotted as functions of time. The vertical guideline in all panels denotes the start time of SSC.
Fig. 2 shows temporal variations of the parameters during a geomagnetic storm, revealing an SSC not accompanied by IP shocks. In this case, SYM-H is initially steady at ~10 nT and suddenly increases at ~02 UT AM by ΔSYM-H = 21 nT during 14 minutes. At the time of SSC (vertical grey guideline in Fig. 2),
To summarize, the time evolution of solar wind parameters around the SSC with IP shocks (Fig. 1) differs from that of the SSC without IP shocks (Fig. 2) in that all three parameters (
Inspired by the above observation of two types of SSCs we examine a larger set of geomagnetic storms. During the period from 1998 to 2008, we select 407 storms with a minimum SYM-H of less than -30 nT. Usually SYM-H is near zero prior to geomagnetic storms, but for some strong events, the index can be negative even before the storms, which we include in the present study. However, we exclude 133 storms that are too weak to identify any SSCs. For the remaining 274 storms, we classify them into four groups according to the existence of SSC and IP shock. Group 1 comprises events with both SSC and IP shock and Group 2 consists of storms that do not have either an SSC or an IP shock. Storms of Group 3 have only SSC without IP shock and storms of Group 4 are associated with only IP shock without SSC.
We classify the SSCs under two different criteria in order to check the sensitivity of the resulting classification to the selection criteria. Our first criterion of SSC is that SYM-H should increase by more than 5 nT in 10 minutes prior to the beginning of the main phase (Kim et al. 2007). The results are shown in Table 1. Storms of Group 3 dominate (41%) and those of Group 1 are ranked second with a fraction of 39%. The fractions of the remaining groups are about 20%. While it is generally known that about 70-80% of SSCs are associated with IP shock, the number of SSCs that are not associated with IP shocks is higher than expected in this study. Only 49% of them (107 out of 220 SSCs) are associated with IP shock. However, only three storms are associated with IP shock but without SSC. The physical parameters of the IP shocks associated with these three storms show relatively smaller increases than those of other IP shocks.
In the second attempt, we modified the criterion of SSC such that SYM-H should increase by 10 nT in 10 minutes. Under this criterion the number of Group 3 storms falls to 28 while that of Group 1 did not change substantially (Table 2). The total number of SSC storms is 131, 79% of which are associated with IP shocks. The results of the latter classification are similar to previous results (Smith et al. 1986; Wang et al. 2006). Since such a selection effect is not the primary goal of the present study, we finally set the criterion as ΔSYM-H >10 nT over 10 minutes for SSC and proceed to the next step of classification of SSCs.
Table 2 also lists the average minimum SYM-H for each group. The average magnitude of storms for Group 1 is the largest, followed by that for Group 3, even though IP shocks are absent. The storms in Groups 2 and 4 have relatively small magnitude of SYM-H regardless of whether IP shocks are present or not.
In order to identify the behavior of physical parameters for Groups 1 and 3, we apply the superposed epoch analysis (O’Brien et al. 2001) to the physical parameters of our interest: SYM-H,
[Fig. 3.] Results of the superposed epoch analysis for Group 1 plotted in the same format as Fig. 1. From the top to bottom panel, B, GSM Bz, Vp, Np, and SYM-H are plotted as functions of the relative time centered at the time of the maximum SYM-H. These parameters are averaged quantities for Group 1 (black curves) and Group 3 (grey curves), respectively.
For Group 1 the solar wind parameters
In Table 3 we list the physical parameters of Group 3, which consists of a total of 28 storms with SSCs defined by an increase of SYM-H by more than 10 nT within 10 minutes. The first four parameters are increments of magnetic field, proton velocity, number density, and dynamic pressure associated with SSCs, as obtained from ACE. The last column shows the source of SSCs, which we determine by referring to the list of ICMEs created by Ian Richardson and Hilary Cane (Near-Earth Interplanetary Coronal Mass Ejections Since January 1996), the list of HSS associated with storms by O. Maris (COMPLEX CATALOGUE of GEOMAGNETIC STORMS-HIGH SPEED STREAMS; 1996 – 2008), and the list of SIRs from Wind and ACE Data during 1995 − 2009 compiled by Jian et al. (2011). Since SIRs are generated by the interaction of relatively slow solar wind and HSS, we mark those events associated with SIR as HSS. Table 3 shows that the most common source for SSCs in Group 3 is HSS.
Fig. 4 summarizes the sources for SSCs in Group 3. HSS contributes to SSC in 21 events and ICME contributes to SSC in 10 events with an overlap between the two contributors. It is remarkable that 6 events are associated with both HSS and ICME. These storms are associated with powerful solar wind and show a very large increase of SSC comparable to storms of Group 1 associated with powerful IP shock. As denoted in the figure, the storms associated with both HSS and ICME have a large increase of SYM-H of 35.3 nT on average. The storms with both ICME and HSS have a larger increase in physical parameters because HSS pushes ICME.
Our interpretation of the result is as follows: when HSS is the main contributor to SSC,
We compare average physical parameters of Group 3 with those of Group 1 in Table 4. To obtain the average values, we selected only those storms for which complete data coverage is available: 64 storms from Group 1 and 23 storms from Group 3, respectively. For each event, the amount of increase in SYM-H and other physical parameters are determined from the interval of SSC.
Group 1 storms show changes of
In this paper we have investigated whether IP shocks are essential for the occurrence of SSCs or some other drivers for SSCs operate. We analyzed 274 geomagnetic storms with a minimum SYM-H of less than –30 nT and changes of solar wind parameters associated with the storms. Selection of SSCs without IP shocks significantly depends on the criterion for SSC: more SSCs without IP shocks are found when weaker storms are included. Since such a selection effect is not the primary goal of the present study, we fixed the criterion of SSC to ΔSYM-H >10 nT over 10 minutes, under which the previous results by Wang et al. (2006) are closely reproduced. We then investigated the simultaneous interplanetary data and obtained the following results.
1. Of the 138 storms with either SSC or IP shocks, 75% are storms accompanied by both SSC and IP shocks (Group 1), 20% are SSCs without IP shocks (Group 3), and 5% are accompanied by IP shocks but without SSCs (Group 4). Additionally we found 136 storms with neither SSCs nor IP shocks (Group 2).
2. Our superposed epoch analysis shows that during Group 1 storms, temporal variations of solar wind parameters,
3. The GSM z-component of the IMF is another important factor for geomagnetic storms. For Group 1 storms,
4. We further checked the association of Group 3 storms with HSS and ICME. We found that 21 of 28 storms result from HSS and 6 of those 21 storms result from HSS and ICME. The latter shows a larger increment of SYM-H.
5. For Group 1 storms, all parameters,
Based on these results, we suggest that the interacting regions between HSS and slower solar wind stream ahead can also compress the magnetosphere to result in local enhancements of the proton number density and the IMF strength. The storms with both ICME and HSS show large increases in physical parameters because HSS pushes ICME. This could explain the aforementioned behaviors of SSCs that occur without IP shocks. IP shocks are therefore an important factor, but not a necessary condition, for SSCs.