The importance of ground magnetic data in specifying the state of magnetosphere–ionosphere coupling: a personal view
© Kamide and Balan. 2016
Received: 21 December 2015
Accepted: 15 February 2016
Published: 10 March 2016
In the history of geomagnetism, geoelectricity and space science including solar terrestrial physics, ground magnetic records have been demonstrated to be a powerful tool for monitoring the levels of overall geomagnetic activity. For example, the Kp and ap indices having perhaps the long-history geomagnetic indices have and are being used as space weather parameters, where “p” stands for “planetary” implying that these indices express average geomagnetic disturbances on the entire Earth in a planetary scale. To quantify the intensity level of geomagnetic storms, however, it is common to rely on the Dst index, which is supposed to show the magnitude of the storm-time ring current. Efforts were also made to inter-calibrate various activity indices. Different indices were proposed to express different aspects of a phenomenon in the near-Earth space. In the early 1980s, several research groups in Japan, Russia, Europe and the US developed the so-called magnetogram-inversion techniques, which were proposed all independently. Subsequent improvements of the magnetogram-inversion algorithms allowed their technology to be applied to a number of different datasets for magnetospheric convection and substorms. In the present review, we demonstrate how important it was to make full use of ground magnetic data covering a large extent in both latitudinal and longitudinal directions. It is now possible to map a number of electrodynamic parameters in the polar ionosphere on an instantaneous basis. By applying these new inverse methods to a number of ground-based geomagnetic observations, it was found that two basic elements in spatial patterns can be viewed as two physical processes for solar wind-magnetosphere energy coupling.
KeywordsGeomagnetic field Magnetic storm and substorm Magnetosphere–ionosphere coupling Geomagnetic activity indices Auroral electrojets Magnetogram inversion Solar wind Loading–unloading process Directly driven process
It is the primary purpose of this paper to review concisely how much the use of ground magnetic observations has contributed to our specification of the energy state of the entire Sun–Earth system. The energy the magnetosphere is gaining from the solar wind for magnetospheric substorms and storms can be estimated from the distribution of electric current vectors in space, which are obtained from geomagnetic disturbances observed on the ground. Different indices were proposed to express different aspects of a particular phenomenon (Sugiura 1964; Mayaud 1980). However, there is no simple way to convert one or one family of geomagnetic indices to other types of different families of indices.
After many years of examining the measured current systems on the basis of the equivalent current systems, several numerical techniques were developed at several institutes independently in recent years, but this concise review deals mainly with the Kamide–Richmond–Matsushita (KRM) and assimilative mapping of ionospheric electrodynamics (AMIE) techniques (Kamide et al. 1981; Richmond and Kamide 1988). Note that it is now possible to map a number of electrodynamic quantities in the entire polar ionosphere on an instantaneous basis. Since field-aligned currents are also derivable from the numerical technique, this “remote sensing” method is quite useful in discussing magnetosphere–ionosphere coupling as well. We will briefly discuss implications of the essential concept and practical procedure of the so-called inversion technique, and will list the advantages and the limitations.
Role of ground-based observations
Although it is in principle impossible to separate accurately the effects of different current sources only through magnetic measurements made on the ground, several powerful inversion techniques were proposed to attempt to separate the effects of different currents in ground magnetic observations. It is also important to clarify the global and local patterns of the ground magnetic perturbations when they are compared with other more direct observations of plasma population, auroras, and electric fields and currents in the ionosphere and magnetosphere.
Until recently, studies were measuring one variable of the entire M–I chain, assuming a second variable, and then calculating the third variable. For example, the electric field was measured, the ionospheric conductivity was assumed, and the current was able to be calculated. Such an approach does not necessarily treat the interactive nature of the mechanism and thus the conclusions from such studies are not unique. By repeating this type of practice, one cannot properly address the basic, complicated, nonlinear problems that treat the luminosity of auroras.
New numerical methods (Mishin 1990; Feldstein and Levitin 1986; Glassmeier 1987) were developed, which coincided with the availability of new systematic magnetometer data. Three numerical schemes were designed to compute not only the global distribution of both ionospheric and field-aligned currents, but also the ionospheric electric fields and Joule heating rate (Fayermark 1977; Kisabeth 1979; Baumjohann et al. 1981; Mishin 1990). Once we understand properly the origins of ground magnetic perturbations in terms of various source currents, ground-based observations have an advantage over “more direct” measurements by radars and satellites, since temporal changes in the geomagnetic field are being monitored continuously at a relatively large number of fixed points on the Earth’s surface. This contrasts to the intrinsic ambiguity in determining the global three-dimensional current system on an individual basis from single satellite passes, which have difficulties separating temporal and spatial changes. For details on the essence of the magnetogram-inversion techniques, see (Kamide and Baumjohann 1993).
What is outstanding about the new methods, such as KRM and AMIE? The magnetogram inversion is instrumental in unifying the information obtained from synoptic observations of geomagnetic fields with the comprehensive in situ observations by spacecraft in magnetospheric research. Usefulness of this method for unveiling polar phenomena in the ionosphere and the corresponding magnetospheric processes has been verified by numerous studies for individual cases that have used these inversion methods. Some of the successful examples which we report can be found in Kamide (1988).
Applications of magnetogram-inversion techniques to polar substorms
The magnetogram-inversion techniques have been shown to be quite mighty and powerful in finding even what causes the auroral electrojets, which is one of the most important elements of magnetospheric substorms. In addition, it would become more powerful if it is combined with other innovative techniques and/or other types of observations.
Regarding the auroral electrojets, they are a specific class of concentrated current flows which are most intense in the region of brightest auroral luminosity. This leads us to the simple view that precipitating energetic particles would enhance ionospheric conductivities, and cause auroras, along with carrying field-aligned currents. If this chain of processes were all genuine, then the growth and decay of the auroral electrojets would be determined by those only of the auroras (Kamide and Richmond 1991; Kamide and Kokubun 1996).
Examination of the recently available simultaneous data from coherent and incoherent radars at high latitudes and polar-orbiting satellites, combined with ground magnetic records, has shown that this is not the case at all. Nature told us that the reality is more complicated. There are systematic overlappings in regions in the polar ionosphere where each of the parameters dominates. On the basis of our knowledge of the spatial–temporal relationship of ionospheric electric fields, currents and conductivities with respect to various forms of auroral luminosities at different substorm phases, an attempt was made to show that within the so-called auroral electrojet there are basically two separate regions, an electric-field-dominant part and a conductivity-dominant part. These two components can be viewed as signaling that two dominant physical processes are operative for solar wind-magnetosphere energy coupling, i.e., the directly driven and the loading–unloading mechanisms. The relative importance of these two components varies significantly, depending on the substorm phases (Kamide 1988). In the following two subsections, we discuss the role of two basic processes in two different topics.
Electric field and conductivity within the auroral electrojets
In this section, it is important to realize that the region of the intense auroral electrojets is neither completely the same as the region of the highest conductivity nor coincides with that of the largest electric field at all local times. One can find many cases where no bright auroras are present even though the electrojet current there is very intense (Nishida and Kamide 1983). It is also important to note that disturbed intervals, that is, increases in the auroral electrojets, do not automatically mean substorm times, although many papers have relied on an operational definition that if the magnitude of the AE index exceeds some threshold value, say several hundred nanoteslas, that interval must be a substorm interval.
Average patterns of ionospheric parameters for different substorm phases
Among a variety of accomplishments of our inversion technique (KRM assimilated), we will show herewith the average patterns of the electrostatic potential and current vectors for different phases. See Kamide and Kokubun (1996) for the outputs in terms of Joule heating and associated field-aligned currents and for the selection of substorms and KRM magnetogram-inversion technique applied to individual substorms. The average pattern of substorm quantities in the polar ionosphere for the different epochs was determined.
In Fig. 2, the typical twin-vortex pattern in terms of the electrostatic potential can be identified, except for the quiet time. There are several points to be noted: (1) The dynamic range in the total potential difference is much smaller than that of the current density. For example, the ratio of the potential between quiet times and the peak substorm time is only 15/55, which can be compared to 20/500 in terms of the maximum electrojet current. This indicates that the electric field is relatively important during quiet times. (2) The difference in the total potential drop across the polar cap between the growth phase and the expansion phase is 2 kV which is only a 7 % increase, even though the difference in terms of the electrojet current is as large as 250 %. Similarly, the decrease in total potential from the peak to the recovery phase of substorms is only 9 %, when the corresponding current decreases considerably by 50 % from 500 to 250 nT. These results clearly demonstrate that a large-scale electric field is dominant not only during the growth phase but also during the recovery phase of substorms. (3) The overall pattern becomes most complicated during the recovery phase of substorms, as the relative size of the high/low potential vortices varies with respect to the substorm phases. The negative potential area on the evening side is larger than the positive potential area on the morning side during the growth phase, but the situation is reversed at the peak epoch. The location of the peak potential is different at different substorm phases as well. With an increase in the electrojet current from the growth phase to the expansion phase, the peak of the high potential vortex approaches the midnight sector, while the peak location of the low potential vortex seems to remain at approximately 15–16 MLT.
Figure 3 shows the distribution of ionospheric current vectors corresponding to the five substorm phases shown in Fig. 2. During the growth phase of substorms, the eastward electrojet expands both latitudinally and longitudinally, and its intensity is almost doubled. The westward electrojet begins to grow during the growth phase and is centered at 0600 MLT. During the growth phase, the intensities of the eastward and westward electrojets are nearly equal. At the expansion onset of a substorm, however, the midnight portion of the westward electrojet is intensified dramatically from less than 0.1 A/m before the expansion onset to nearly 0.4 A/m after the onset; however, its morning portion remains almost the same. At the maximum epoch of substorms, the westward electrojet extends over a wide MLT range including the evening sector where it intrudes into the region poleward from the eastward electrojet.
We can recognize that the substorm westward electrojet peaks in the midnight sector, reaching 0.6 A/m, where the maximum H perturbation on the ground is 500 nT. It is significant that most of the changes in the current system occur between 1800 and 0600 MLT, like an addition of an intense westward current in the dark sector. During the recovery phase, the ionospheric current pattern becomes very much like that during the growth phase. The overall current system now consists of a pair of electrojets centered at dusk and dawn. However, one significant difference between the growth-phase and recovery-phase patterns is that during the recovery phase, both electrojets are connected to the cusp currents on the dayside. That is, the eastward electrojet is contiguous to the dayside eastward current located on the equatorward side of the westward current, which then joins the morning side westward electrojet.
An important point to be confirmed is that there are essentially two modes to the westward electrojet, one in which the contributions to the electrojet magnitude are “conductivity dominant,” and one in which they are “electric field dominant.” The exact classification into these two modes during substorms using observed data is rather difficult, however, because the corresponding currents are contiguous everywhere in the electrojet. It has been shown statistically that the westward electrojet near midnight and in the early morning hours is characterized mainly by the relatively high Hall conductivity, whereas the westward electrojet in the late morning sector is dominated by the large southward electric field. The latter behavior is similar to that of the eastward electrojet in the evening sector, although the sense of the electric field is of course reversed.
Although it has been a common practice to assume that the westward electrojet during substorms is associated with a conductivity enhancement, a part of the westward electrojet in the later morning sector can in fact be intensified without having high conductivity values. This indicates that the electric field and the conductivity within the auroral electrojet are not in constant proportion in all locations. These characteristics of the relative function of the electric field and the conductance are extremely important because many researchers have tacitly assumed that the auroral electrojet, as the terminology implies, flows in the region of high auroral activity where the ionospheric conductivity is highest.
We contend that the possibility of there being two types of high-latitude current systems might have been implicit in some of the earlier studies that relied only on ground-based magnetic observations (Pytte et al. 1978). Two types of polar current systems, DP 1 and DP 2, have been proposed (Nishida and Kamide 1983). DP 2 consists of the eastward electrojet centered in the evening sector and the westward electrojet centered in the late morning sector, while DP 1 is dominated by the westward electrojet in the midnight sector. It is important to note that these two modes do coexist at all times during disturbed periods and that the relative strength of these two current systems varies from time to time, making individual current patterns very complicated.
These two components can be identified as the signatures for the directly driven and the unloading processes, respectively. The auroral electrojets associated with direct energy input from the solar wind into the magnetosphere flow primarily in the dusk and dawn sectors and increase in association with enhanced convection. The effect of this energy input has been described in terms of an enhancement of the DP 2 system. This is a typical signature for the substorm growth phase which precedes the expansion phase onset.
Unloading of energy stored in the tail during the growth phase leads to the formation of the intense westward electrojet in the midnight sector during the expansion phase of a substorm. This westward electrojet is controlled by high conductivity in the midnight sector, rather than a strong electric field. The enhancement in the conductivities, particularly the Hall conductivity, results from an enhanced ionization caused by accelerated electrons, reflecting the unloading of energy from the magnetotail. It is important to emphasize that the directly driven component is present throughout the entire lifetime of a substorm, indicating that the solar wind energy is continuously fed to the magnetosphere, though with varying degrees. This component becomes, therefore, relatively dominant again during the late recovery phase as the unloading component wanes.
Historically, magnetic records obtained from the ground have widely been used to study physical processes that occur in the near-Earth environment. Over the last two hundred years, this type of study about the structure and temporal changes of the Sun–Earth space is now called space weather since the magnetic data obtained at the Earth’s surface include much valuable information concerning various source currents. In fact, the study of space weather began as examining geomagnetic disturbances during geomagnetic storms. Other instruments, such as balloons, rockets, satellites, and radars, are all big in size, expensive to construct or install compared to inexpensive magnetometers. For this reason, scientists think that it is extremely difficult to separately evaluate the relative strength and importance of these currents in generating the particular modes of global or local magnetic disturbances that are to be studied in detail.
It is not too much to say that Kamide and coworkers have brought more than the KRM algorithm as a method and its applications to space research. They have studied the growth and decay of the ring current during magnetic storms. They have also examined the influence of the interplanetary magnetic field (IMF) on the ring current and substorm processes, finding that the IMF polarity determines not only the intensity but also the occurrence probability of substorms. They have used electron precipitation data from polar-orbiting satellites to identify the auroral belt. One of their findings from this extensive study has become a standard model of the size of the belt, which is controlled by the IMF and substorms.
Using the KRM method, it has been demonstrated that the auroral electrojet consists of two major components, i.e., the electric field-dominant and the conductivity-dominant currents, and that their relative importance varies with substorm phases. It has been shown how the current and potential grow/decay in the ionosphere in response to changes in the solar wind. This method has proved to be quite useful for unifying the information obtained from synoptic observations of geomagnetic field with the comprehensive in situ observations by spacecraft. The usefulness of this method has been testified by numerous case studies. The KRM (and AMIE) method is now playing a key role even in real-time calculations in space weather predictions as well. This specification gives boundary conditions to other simulation schemes about the state of the magnetosphere, ionosphere, and thermosphere.
In a sense, the invention of magnetogram-inversion techniques can be treated as a revolution regarding the role of ground magnetic observations. These techniques help deriving the three-dimensional current system and global ionospheric potential pattern from ground-based magnetic observations. Using this inversion method, Kamide and coworkers have demonstrated that the auroral electrojet consists of two major components, i.e., the electric field-dominant and the conductivity-dominant currents, and that the balance of these components varies with substorm phases. They have also shown how the current and potential develop in the magnetosphere and ionosphere in response to variations in the solar wind. In other words, the development of the KRM method “elevated” geomagnetism to a quantitative measure of the state of the magnetosphere–ionosphere system.
Finally, we caution that the use of ground magnetic data to obtain successively magnetospheric and ionospheric parameters must go through a number of assumptions. The most serious assumption in the KRM algorithm is that one has to assume the distribution of the ionospheric conductance, but there are, at present, no measurements of the global ionospheric conductivities available in real time. Therefore, Kamide and colleagues utilized various models of the ionospheric conductance obtained, for example, by using incoherent scatter radars and satellite measurements of X-ray and UV auroras. We note that the obtained ionospheric currents are not very sensitive to the choice of the ionospheric conductances. Furthermore, in practically solving numerically the complicated equations of the KRM method, it is assumed that magnetic field lines are all vertical to the Earth’s surface, simplifying the numerical scheme in calculating the electric potential. Limitations of the inversion techniques are described in more detail in Kamide et al. (1981).
YK prepared the first draft of the review paper. YK and NB together discussed and prepared the final version of the paper.
We thank the members of the 2015 AOGS Program Committee for encouraging us to write a concise review on this topic.
The authors have no competing interest in the publication of this article.
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