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Erhan Kudeki - One of the best experts on this subject based on the ideXlab platform.
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estimating daytime vertical exb drift velocities in the equatorial f region using ground based magnetometer observations
Geophysical Research Letters, 2002Co-Authors: David T Anderson, A Anghel, K Yumoto, Mutsumi Ishitsuka, Erhan KudekiAbstract:[1] The daytime equatorial electrojet is a narrow band of enhanced eastward current flowing in the 100 to 120 km altitude region within ±2° latitude of the dip equator. A unique way of determining the daytime strength of the electrojet is to observe the difference in the magnitudes of the Horizontal (H) component between a magnetometer placed directly on the magnetic equator and one displaced 6 to 9 degrees away. The difference between these measured H values provides a direct measure of the daytime electrojet current, and in turn, the magnitude of the vertical ExB drift velocity in the F region ionosphere. This paper discusses a recent study that has established the quantitative relationship between the vertical ExB drift velocity in the ionospheric F region and the daytime strength of the equatorial electrojet in the South American (west coast) longitude sector.
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estimating daytime vertical exb drift velocities in the equatorial f region using ground based magnetometer observations
Geophysical Research Letters, 2002Co-Authors: David R Anderson, K Yumoto, A Anghel, Mutsumi Ishitsuka, Erhan KudekiAbstract:[1] The daytime equatorial electrojet is a narrow band of enhanced eastward current flowing in the 100 to 120 km altitude region within ±2° latitude of the dip equator. A unique way of determining the daytime strength of the electrojet is to observe the difference in the magnitudes of the Horizontal (H) component between a magnetometer placed directly on the magnetic equator and one displaced 6 to 9 degrees away. The difference between these measured H values provides a direct measure of the daytime electrojet current, and in turn, the magnitude of the vertical ExB drift velocity in the F region ionosphere. This paper discusses a recent study that has established the quantitative relationship between the vertical ExB drift velocity in the ionospheric F region and the daytime strength of the equatorial electrojet in the South American (west coast) longitude sector.
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Plasma wave excitation on meteor trails in the equatorial electrojet
Geophysical Research Letters, 1994Co-Authors: Elaine Chapin, Erhan KudekiAbstract:The unusual properties of meteor echoes recently observed at Jicamarca [Chapin and Kudeki, 1994] are attributed to the growth and propagation of plasma irregularities along meteor trails deposited within the equatorial electrojet. It is suggested that trails at electrojet heights must carry intense discharge currents that excite two-stream and/or gradient drift instabilities for irregularity growth. The direction of electron motion responsible for the discharge current agrees with the Doppler shift of the high frequency components in meteor echo signals.
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radar interferometric imaging of field aligned plasma irregularities in the equatorial electrojet
Geophysical Research Letters, 1991Co-Authors: Erhan Kudeki, Fahri SurucuAbstract:A multiple-receiver radar technique for imaging the spatial distribution of ionospheric plasma irregularities is introduced and demonstrated with equatorial electrojet data obtained at the Jicamarca Radio Observatory. The images obtained with a few seconds time resolution enable the monitoring of the temporal evolution of the irregularity structures within the radar field of view. Daytime electrojet images contain signatures of localized irregularity patches which drift in the east-west direction at about the ion-acoustic velocity.
K Yumoto - One of the best experts on this subject based on the ideXlab platform.
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the response of the dayside equatorial electrojet to step like changes of imf bz
Journal of Geophysical Research, 2013Co-Authors: S Ohtani, T Uozumi, Hideaki Kawano, Akimasa Yoshikawa, Hisashi Utada, Tsutomu Nagatsuma, K YumotoAbstract:[1] The equatorial electrojet (EEJ) is driven by zonal electric fields, which are known to be well correlated with the interplanetary electric field and therefore with the interplanetary magnetic field (IMF) BZ component. In the present study, we investigate how the equatorial H magnetic component, and therefore the EEJ, responds to step-like changes of IMF BZ. The reduction of southward IMF BZ (northward turning) and that of northward IMF BZ (southward turning) are examined separately. The result shows that for the northward turnings, the EEJ immediately starts to weaken with the accuracy of the estimates of the travel times of the IMF changes. The time constant of the response is much longer, and the equatorial H component decreases continuously by 40 nT for 30 min after the northward turnings. In contrast, the response of the EEJ to the southward turnings is far less clear in both magnitude and timing, and it does not depend on whether or not IMF BZ actually becomes southward. The difference in the EEJ response to the northward and southward turnings reflects at least partially the fact that the magnetosphere-ionosphere system is more sensitive to IMF BZ when IMF is southward than northward. It is suggested that the electric field penetrates from the polar region to the dip equator through a global current system that connects the auroral Electrojets and the EEJ, and the ionospheric conductance in the polar region may play an important role in the formation of such a current system.
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characteristics of equatorial electrojet over india determined from a thick current shell model
Journal of Atmospheric and Solar-Terrestrial Physics, 2013Co-Authors: A B Rabiu, C A Onwumechili, Nandini Nagarajan, K YumotoAbstract:Abstract For the first time the five parameters required to fully describe Onwumechili’s composite thick current shell model format of equatorial electrojet have been evaluated from a single autonomous set of ground data at solar minimum. The thick current shell model, which takes into account the vertical ionospheric currents, permits both the width and the thickness of the jet to be determined simultaneously. The mean annual values of the electrojet parameters evaluated over India sector are: the peak intensity of the forward current at its centre, 62.97±2.73 A/km; the peak intensity of the return current, 19.43±2.49 A/km; the ratio of the peak return to the peak forward current intensity, 0.312±0.052; the total forward current flowing between the current foci, 19.01±1.74 kA; half of the latitudinal width or the focal distance from the current centre, 2.7±0.18°; the distance of the peak return current location from the current centre, 5.31±0.19°; the half thickness of the peak current density, 0.063±0.003°; the latitudinal extent of the current from its centre, 9.25±2. 08°; and the dip latitude of the equatorial electrojet EEJ centre −0.190±0.003°. The dip latitude of the centre of EEJ exhibits a consistent northward migration towards the dip equator from the rising of the jet at dawn from an annual average of −0.193° to about −0.186° at about 1100 h LT, after which it begins to recede southward towards the dusk. Our results show that the electrojet becomes more (less) intensified as the centre of the electrojet moves northwards (southwards) towards (away from) the dip equator. The diurnal variation of the thickness of the EEJ is opposite that of its current intensity and half width. The thickness of equatorial electrojet EEJ exhibits a consistent diurnal variation such that it decreases from about 0.066° at dawn to the minimum at about 1100 h LT and then begins to increase towards the dusk. The wider (thicker) the EEJ, the stronger (weaker) the EEJ strength. The order of seasonal variation of the mean daytime current intensity Jo and forward current Ifwd is E>D>J. However, the diurnal variations of the EEJ parameters exhibit seasonal dependence as the order of seasonal variation is not uniform at every hour of daytime for all the parameters.
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development of auroral Electrojets and low latitude geomagnetic disturbances during strong magnetic storms on november 7 11 2004
Cosmic Research, 2011Co-Authors: S I Solovyev, R N Boroev, A V Moiseev, K YumotoAbstract:The influence of auroral electojets and solar wind parameters on variations in low-latitude geomagnetic disturbances and Dst during strong magnetic storms on November 7–8, 2004 with Dst ≈ −380 nT and on November 9–10, 2004 with Dst ≈ −300 nT is studied on the basis of global geomagnetic observations. It is found that the impulsive variations of the western electrojet intensity with a duration of Δt ≈ 1–2 h (probably, substorm disturbances) lead to positive low-latitude disturbances of ΔH at Φ′ ≈ 10°–30° and to disturbances of the same durations with an amplitude +ΔH ∼ 30–100 nT at latitudes of the polar cap (Φ′ ≈ 75°–80°). More durable (with Δt ≥ 10 h) convection Electrojets whose centers are shifted to latitudes of ∼50°–55° in the process of storm development are the main cause of the increase in negative values of ΔH at low latitudes and Dst. It is shown that meridional dynamics of position of the center of Electrojets and the equatorial boundary of the auroral oval is governed by variations (increase or decrease) in the intensity of negative values of the IMF Bz component. It is assumed that in these storms the intensification of the magnetospheric partially ring current closes the circuit to the ionosphere with the help of field-aligned currents at the equatorial boundary of the auroral oval is the main cause of the magnetic field depression at low latitudes.
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a new index to monitor temporal and long term variations of the equatorial electrojet by magdas cpmn real time data ee index
Earth Planets and Space, 2008Co-Authors: T Uozumi, K Kitamura, K Yumoto, Hideaki Kawano, Akimasa Yoshikawa, Shuji Abe, Yoshihiro Kakinami, M Shinohara, T Ueno, T TokunagaAbstract:A new index, EE-index (EDst, EU, and EL), is proposed to monitor temporal and long-term variations of the equatorial electrojet by using theMAGDAS/CPMN real-time data. The mean value of the H component magnetic variations observed at the nightside (LT = 18–06) MAGDAS/CPMN stations along the magnetic equatorial region is found to show variations similar to those of Dst; we defined this quantity as EDst. The EDst can be used as a proxy of Dst for the real-time and long-term geospace monitoring. By subtracting EDst from the H component data of each equatorial station, it is possible to extract the Equatorial Electrojet and Counter Electrojet components, which are defined as EU and EL, respectively.
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characteristics of the equatorial electrojet current in the central region of south america
Earth Planets and Space, 2008Co-Authors: R. G. Rastogi, H. Chandra, K Kitamura, M E James, K YumotoAbstract:We describe here for the first time the morphology of the equatorial electrojet (EEJ) in the Central American Sector based on an analysis of the geomagnetic field components from six stations distributed on both sides of the dip equator along the 60°W geographic longitude sector. Diurnal and latitudinal variations in the horizontal and vertical components are shown to follow the Chapman model of EEJ. The horizontal component vector due to the ionospheric current aligned itself close to magnetic north, with a mean Declination of 10°W (ranging from 9°W to 14°W). There was a significant counter-electrojet effect before sunrise at stations close to the dip equator, suggesting late reversal of solar-quiet (Sq) electric field in the morning hours. The observed variations in the magnetic meridional current did not seem to be associated with EEJ currents. The centre of the electrojet was around 0.25°S of the dip equator in the morning hours and shifted gradually to 1.5°S by the evening hours. Magnetic storms occurring during the midday hours produced an exceptionally large decrease in the H (horizontal component) field at stations close to the dip equator.
J H Shue - One of the best experts on this subject based on the ideXlab platform.
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effects of solar wind density on the auroral Electrojets and global auroras during geomagnetic storms
Geophysical monograph, 2013Co-Authors: Y. Kamide, J H Shue, M BrittnacherAbstract:It was shown statistically, some thirty years ago, that substorms occurring during the initial phase of geomagnetic storms and those during the main phase are different in character. Substorms during geomagnetic storms, regardless of the phases in which they occur, were also shown to be different from normal isolated substorms in terms of the relative strength between the eastward and westward auroral Electrojets. Based on the intensities of the auroral Electrojets estimated from ground magnetometer data and on the distribution of large-scale auroras seen in Polar auroral images, the present study shows that the solar wind density does in fact control the intensity of the auroral Electrojets and the associated auroral activity, but the efficiency of the control depends strongly on the polarity of interplanetary magnetic field (IMF). The earlier statistical results can consistently be accounted for by considering that the initial phase of geomagnetic storms is caused by the high dynamic pressure (or density) of the solar wind, while southward IMF dominates the main phase.
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a systematic study of effects of solar wind density on auroral Electrojets
Geophysical Research Letters, 2005Co-Authors: Y. Kamide, J H Shue, P T NewellAbstract:[1] The subject of effects of solar wind density (Np) on auroral Electrojets has recently received increasing attention. For “unbiased” events in which only Np varied significantly but other solar wind parameters were relatively constant, we calculated rates of change of the auroral Electrojets per unit change of Np (dAU/dNp and dAL/dNp). Here we report that the distribution of dAU/dNp and dAL/dNp binned by the Z component of interplanetary magnetic field (IMF) shows a butterfly pattern. The rates are found to be small for northward IMF. As the southward IMF becomes larger, the distribution bifurcates–one branch extending to positive rates and the other to negative rates. Although it has been commonly believed that the enhanced Np increases the auroral Electrojets, the enhanced Np can also decrease the auroral Electrojets with a 49% probability.
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solar wind density and auroral Electrojets during geomagnetic storms
Cospar Colloquia Series, 2002Co-Authors: Y. Kamide, J H Shue, M BrittnacherAbstract:ABSTRACT It was shown statistically, some 30 years ago, that substorms occurring during the initial phase of geomagnetic storms and those during the main phase are different in character. Based on the intensities of the auroral Electrojets estimated from ground magnetometer data, we show that the solar wind density controls the intensity of the auroral Electrojets, but the efficiency of the control depends strongly on the polarity of interplanetary magnetic field (IMF). The earlier statistical results can consistently be accounted for by considering that the initial phase of geomagnetic storms is caused by the high dynamic pressure, i.e., density, of the solar wind while southward IMF dominates the main phase.
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effects of solar wind density on auroral Electrojets
Geophysical Research Letters, 2001Co-Authors: J H Shue, Y. KamideAbstract:During the magnetic cloud event of January 10–11, 1997, several density enhancements in the solar wind were observed while other solar wind parameters were relatively constant. By using this fortuitous opportunity, the effects of the solar wind density on the intensity of the auroral Electrojets are examined. It is found that a positive relationship exists between the solar wind density and the intensity of the auroral Electrojets. The relationship is found to be much weaker for northward interplanetary magnetic field (IMF) than for southward IMF. It is also shown that when the IMF is directed southward, the density effect is dominant in the westward electro jet, while it is most effective in the eastward electro jet when the IMF is directed northward.
Y. Kamide - One of the best experts on this subject based on the ideXlab platform.
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effects of solar wind density on the auroral Electrojets and global auroras during geomagnetic storms
Geophysical monograph, 2013Co-Authors: Y. Kamide, J H Shue, M BrittnacherAbstract:It was shown statistically, some thirty years ago, that substorms occurring during the initial phase of geomagnetic storms and those during the main phase are different in character. Substorms during geomagnetic storms, regardless of the phases in which they occur, were also shown to be different from normal isolated substorms in terms of the relative strength between the eastward and westward auroral Electrojets. Based on the intensities of the auroral Electrojets estimated from ground magnetometer data and on the distribution of large-scale auroras seen in Polar auroral images, the present study shows that the solar wind density does in fact control the intensity of the auroral Electrojets and the associated auroral activity, but the efficiency of the control depends strongly on the polarity of interplanetary magnetic field (IMF). The earlier statistical results can consistently be accounted for by considering that the initial phase of geomagnetic storms is caused by the high dynamic pressure (or density) of the solar wind, while southward IMF dominates the main phase.
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effects of solar wind density on auroral Electrojets and brightness under influence of substorms
Annales Geophysicae, 2009Co-Authors: Jihhong Shue, Y. Kamide, J W GjerloevAbstract:Using the auroral electrojet indices and Polar Ultraviolet Imager auroral images, we examined two fortuitous events during which the solar wind density had clear enhancements while the other solar wind parameters were relatively constant. Two electrojet enhancements were found in each event. The first electrojet enhancement was likely to be related to a substorm in which an auroral bulge appeared at premidnight. The second electrojet enhancement was driven by the density enhancement in the solar wind. The auroral oval became wider in latitude and the auroral distribution became dispersed after the density enhancement arrived at the Earth. The total auroral power integrated over the entire nightside region from 50 to 80° MLAT, however, did not increase significantly in response to the density enhancement. Our interpretation is that the substorm that occurred prior to the solar wind density enhancement had drained out a significant portion of the stored energy in the magnetotail; therefore, less precipitation energy was deposited into the auroral ionosphere by the density enhancement.
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a systematic study of effects of solar wind density on auroral Electrojets
Geophysical Research Letters, 2005Co-Authors: Y. Kamide, J H Shue, P T NewellAbstract:[1] The subject of effects of solar wind density (Np) on auroral Electrojets has recently received increasing attention. For “unbiased” events in which only Np varied significantly but other solar wind parameters were relatively constant, we calculated rates of change of the auroral Electrojets per unit change of Np (dAU/dNp and dAL/dNp). Here we report that the distribution of dAU/dNp and dAL/dNp binned by the Z component of interplanetary magnetic field (IMF) shows a butterfly pattern. The rates are found to be small for northward IMF. As the southward IMF becomes larger, the distribution bifurcates–one branch extending to positive rates and the other to negative rates. Although it has been commonly believed that the enhanced Np increases the auroral Electrojets, the enhanced Np can also decrease the auroral Electrojets with a 49% probability.
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solar wind density and auroral Electrojets during geomagnetic storms
Cospar Colloquia Series, 2002Co-Authors: Y. Kamide, J H Shue, M BrittnacherAbstract:ABSTRACT It was shown statistically, some 30 years ago, that substorms occurring during the initial phase of geomagnetic storms and those during the main phase are different in character. Based on the intensities of the auroral Electrojets estimated from ground magnetometer data, we show that the solar wind density controls the intensity of the auroral Electrojets, but the efficiency of the control depends strongly on the polarity of interplanetary magnetic field (IMF). The earlier statistical results can consistently be accounted for by considering that the initial phase of geomagnetic storms is caused by the high dynamic pressure, i.e., density, of the solar wind while southward IMF dominates the main phase.
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effects of solar wind density on auroral Electrojets
Geophysical Research Letters, 2001Co-Authors: J H Shue, Y. KamideAbstract:During the magnetic cloud event of January 10–11, 1997, several density enhancements in the solar wind were observed while other solar wind parameters were relatively constant. By using this fortuitous opportunity, the effects of the solar wind density on the intensity of the auroral Electrojets are examined. It is found that a positive relationship exists between the solar wind density and the intensity of the auroral Electrojets. The relationship is found to be much weaker for northward interplanetary magnetic field (IMF) than for southward IMF. It is also shown that when the IMF is directed southward, the density effect is dominant in the westward electro jet, while it is most effective in the eastward electro jet when the IMF is directed northward.
Y I Feldstein - One of the best experts on this subject based on the ideXlab platform.
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Spiral structures and regularities in magnetic field variations and auroras
Copernicus Publications, 2012Co-Authors: Y I Feldstein, L I Gromova, M. Förster, A E LevitinAbstract:The conception of spiral shaped precipitation regions, where solar corpuscles penetrate the upper atmosphere, was introduced into geophysics by C. Störmer and K. Birkeland at the beginning of the last century. Later, in the course of the XX-th century, spiral distributions were disclosed and studied in various geophysical phenomena. Most attention was devoted to spiral shapes in the analysis of regularities pertaining to the geomagnetic activity and auroras. <br><br> We review the historical succession of perceptions about the number and positions of spiral shapes, that characterize the spatial-temporal distribution of magnetic disturbances. We describe the processes in the upper atmosphere, which are responsible for the appearance of spiral patterns. We considered the zones of maximal aurora frequency and of maximal particle precipitation intensity, as offered in the literature, in their connection with the spirals. <br><br> We discuss the current system model, that is closely related to the spirals and that appears to be the source for geomagnetic field variations during magnetospheric substorms and storms. The currents in ionosphere and magnetosphere constitute together with field-aligned (along the geomagnetic field lines) currents (FACs) a common 3-D current system. At ionospheric heights, the westward and eastward Electrojets represent characteristic elements of the current system. The westward electrojet covers the longitudinal range from the morning to the evening hours, while the eastward electrojet ranges from afternoon to near-midnight hours. The polar electrojet is positioned in the dayside sector at cusp latitudes. All these Electrojets map along the magnetic field lines to certain plasma structures in the near-Earth space. The first spiral distribution of auroras was found based on observations in Antarctica for the nighttime-evening sector (N-spiral), and later in the nighttime-evening (N-spiral) and morning (M-spiral) sectors both in the Northern and Southern Hemispheres. The N- and M-spirals drawn in polar coordinates form an oval, along which one observes most often auroras in the zenith together with a westward electrojet. <br><br> The nature of spiral distributions in geomagnetic field variations was unabmibuously interpreted after the discovery of the spiral's existence in the auroras had been established and this caused a change from the paradigm of the auroral zone to the paradigm of the auroral oval. Zenith forms of auroras are found within the boundaries of the auroral oval. The oval is therefore the region of most frequent precipitations of corpuscular fluxes with auroral energy, where anomalous geophysical phenomena occur most often and with maximum intensity. <br><br> S. Chapman and L. Harang identified the existence of a discontinuity at auroral zone latitudes (Φ ∼ 67°) around midnight between the westward and eastward Electrojets, that is now known as the Harang discontinuity. After the discovery of the auroral oval and the position of the westward electrojet along the oval, it turned out, that there is no discontinuity at a fixed latitude between the opposite Electrojets, but rather a gap, the latitude of which varies smoothly between Φ ∼ 67° at midnight and Φ ∼ 73° at 20:00 MLT. In this respect the term ''Harang discontinuity'' represents no intrinsic phenomenon, because the westward electrojet does not experience any disruption in the midnight sector but continues without breaks from dawn to dusk hours
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high latitude Electrojets and auroral luminosity and auroral particle precipitations
Physics of Auroral Phenomena XXX Annual Seminar Apatity 2007, 2007Co-Authors: Y I Feldstein, A Prigancova, V G Vorobjev, Judy Cumnock, G V Starkov, O I Yagodkina, Lars BlombergAbstract:The mutual location of high-latitude Electrojets, typical regions of the auroral luminosity and regions of auroral energy particle participations into the upper atmosphere under substorm conditions are considered. Three Electrojets exist at high latitudes during substorm intervals: WE - westward electrojet, EE - eastward electrojet and PE - polar electrojet. Geomagnetic latitudes of the WE/EE and PE location vary depend on local time and magnetic activity level, respectively. It is shown that the WE is located within the limits of the auroral oval precipitation (AOP), the EE in the evening sector is located within the diffuse auroral zone (DAZ) and the PE near noon is located at the poleward AOP boundary shifting poleward with decreasing the magnetic activity level. The relationship of Electrojets with different plasma domains in the magnetosphere is discussed.
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auroral Electrojets and 3d currents in the ionosphere magnetosphere system
Physics of Auroral Phenomena XXIX Annual Seminar Apatity 2006, 2006Co-Authors: Y I Feldstein, A Prigancova, Judy Cumnock, Lars Blomberg, V A Popov, J U Kozyra, B T Tsurutani, L I Gromova, A E LevitinAbstract:There are shortly described results of the analysis of variations in the location and intensity of the auroral Electrojets during magnetic storms and substorms using a numerical method for estimating the equivalent ionospheric currents based on data from meridian chains of magnetic observatories. It is shown that the westward electrojet adjoins to the polar electrojet located at cusp latitudes in the dayside sector. The association of Electrojets with the field-aligned currents (FACs), namely Region 1 FAC and Region 2 FAC is considered. During intense disturbances a Region 3 FAC (accompanied with diffuse electron precipitation from the plasma sheet boundary layer) with the downward current was identified. The analysis of observational data is summarized in terms of 2D time-latitude distribution of Electrojets at ionospheric altitudes. The magnetic field sawtooth variations generated during the storm main and early recovery phases are also discussed. To follow 3D currents in the magnetosphere- ionosphere system a clarified view of interrelated 3D currents and magnetospheric plasma domains is presented.
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about the relationship between auroral Electrojets and ring currents
Annales Geophysicae, 2000Co-Authors: A Grafe, Y I FeldsteinAbstract:The relationship between the storm-time ring current and the auroral Electrojets is investigated using IMAGE magnetometer data, DSt and H-SYM, and solar wind data. Statistical results as well as the investigation of single events show that the auroral Electrojets occur also during nonstorm conditions without storm-time ring current development and even during the storm recovery phase of increasing DSt. A close correlation between electrojet intensity and ring current intensity was not found. Though the eastward electrojet moves equatorward during the storm main phase there is no unequivocal relationship between the movement of the westward electrojet and the ring current development. All these results suggest that the auroral Electrojets and the ring current develop more or less independently of each other.
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dynamics of the auroral Electrojets and their mapping to the magnetosphere
Radiation Measurements, 1999Co-Authors: Y I Feldstein, A Grafe, L I Gromova, C I Meng, V V Kalegaev, I I Alexeev, Yu P SumarukAbstract:Abstract Data of the EISCAT and IMAGE magnetic observatories chains in combination with data of three Russian observatories (St. Petersburg, Borok and Moscow) were used to determine the eastward and westward electrojet dynamics in the course of magnetic storms. During the storm main phase and maximum substorm intensity the eastward electrojet is located at latitudes lower than usual. During intervals between substorms the westward electrojet centre shifts equatorwards as Dst increases. At a substorm maximum the westward electrojet widens polewards. The spectrograms of precipitating electrons and ions of auroral energies obtained onboard the DMSP F8, F10 and F11 satellites allow to connect the regions of the electrojet location with characteristic plasma structures at ionospheric altitudes. The eastward electrojet in the evening sector is located in the region of diffuse electron precipitations. The electrojet centre coincides with the latitude of an energy flux maximum of auroral protons. In the course of substorms the westward electrojet at the nightside is located at latitudes of both diffuse and discrete electron precipitations. The Electrojets and plasma region boundaries are mapped to the magnetosphere. The paraboloid model of the magnetosphere is used here. The influence of paraboloid model input parameters on the dayside cusp latitude, on the ionospheric boundaries between open and closed as well as dipole-like and tail-like field lines is considered. It is shown that tail currents influence magnetic field line configuration in the nightside magnetosphere stronger than the ring current.