Magnetospheric ULF wave activity monitoring based on the ULF-index OLGA KOZYREVA and N. Kleimenova Institute of the Earth Physics, RAS.

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Magnetospheric ULF wave activity monitoring based on the ULF-index OLGA KOZYREVA and N. Kleimenova Institute of the Earth Physics, RAS

Various geomagnetic indices (Kp, Ap, Dst, SYM-H, AE, AU, AL, PC, etc.) characterize the level of the electrodynamics of the near- Earth environment. However, there was no index for the wave activity monitoring. Various geomagnetic indices (Kp, Ap, Dst, SYM-H, AE, AU, AL, PC, etc.) characterize the level of the electrodynamics of the near- Earth environment. However, there was no index for the wave activity monitoring. We developed the special index of the dayside ULF wave activity in order to estimate the level of low-frequency turbulence, which we called “ ULF- index ”. We developed the special index of the dayside ULF wave activity in order to estimate the level of low-frequency turbulence, which we called “ ULF- index ”. The most promising frequency range for the index definition is the Pc5 band (~ 2-7 mHz) with the most intense fluctuations is of key importance. The most promising frequency range for the index definition is the Pc5 band (~ 2-7 mHz) with the most intense fluctuations is of key importance.ULF-index

The wave index as a proxy of global ULF activity is reconstructed from the 1- min data of the magnetic stations arrays in Northern hemisphere: The wave index as a proxy of global ULF activity is reconstructed from the 1- min data of the magnetic stations arrays in Northern hemisphere: INTERMAGNETINTERMAGNET Greenland ArraysGreenland Arrays MACCSMACCS 210 Magnetic Meridian Chain210 Magnetic Meridian Chain Russian Arctic magnetic stationsRussian Arctic magnetic stations DMI WDC observatoriesDMI WDC observatories ULF-index O. Kozyreva,V. Pilipenko, M. Engebretson et al., Planetary and Space Science, 2007, 55, pp.755–769. O. Kozyreva, V. Pilipenko, M. Engebretson et al., Planetary and Space Science, 2007, 55, pp.755–769.

BASE VERSION  f  mHz MLT   Pc5 / Pi ° 60-70° 70-90° MLT MLT NEW MLT ftp://space.augsburg.edu/MACCS/ULF_Index/ ftp://space.augsburg.edu/MACCS/ULF_Index/ We upgraded the base version of ULF- index and applied it to Pc5/Pi3 pulsations study in different MLT sectors and different ranges of geomagnetic latitudes during the different phases of strong magnetic storms: We upgraded the base version of ULF- index and applied it to Pc5/Pi3 pulsations study in different MLT sectors and different ranges of geomagnetic latitudes during the different phases of strong magnetic storms: -150 nT < Dst min < -100 nT -150 nT < Dst min < -100 nT Geomagnetic pulsations at frequencies of ~2–7 mHz are the most typical oscillations in the geomagnetic field. They are represented by quasi- sinusoidal Pc5 in the morning–daytime and impulsive bursts of Pi3 in the evening–nighttime sector. The amplitude of these pulsations is maximal in the auroral zone and shifts toward lower latitudes with increasing magnetic activity. In the initial phase of strong magnetic storms maximum of ULF activity is mainly observed in the morning- dayside polar cap.

For an analysis we selected 19 strong isolated storms (in ) that continued for not more than two days. We used the superposed epoch technique. A “zero” epoch is the UT when Dst-index reached minimal value during main phase. We have analyzed the time interval of 48 hours for the each selected storms, i.e. 24 hours before and 24 hours after the Dst minimum.

RESULTS of statistical analysis In polar latitudes the ULF- index is maximal in the morning in all phases of magnetic storms. In polar latitudes the ULF- index is maximal in the morning in all phases of magnetic storms. In auroral latitudes the ULF-index demonstrates a strong maximum in the morning in the main phases of magnetic storms. In the initial and recovery phases, the morning ULF activity (Pc5) is comparable with the night ULF activity (Pi3). In auroral latitudes the ULF-index demonstrates a strong maximum in the morning in the main phases of magnetic storms. In the initial and recovery phases, the morning ULF activity (Pc5) is comparable with the night ULF activity (Pi3). In subauroral latitudes the enhancement of night-side ULF activity could be a result of the auroral magnetic activity shifting to lower latitudes in the main phase of storms. In subauroral latitudes the enhancement of night-side ULF activity could be a result of the auroral magnetic activity shifting to lower latitudes in the main phase of storms.

As the typical example, we consider a strong magnetic storm on May The morning ULF activity in polar and auroral zones abruptly increases with the beginning of the main phase of storm (~07 UT). The ULF- index values are much higher in the morning than in the night. The second burst of ULF activity is observed at storm development maximum.

The top map is plotted for UT corresponding to the first peak of the ULF-index, the bottom map (14-16 UT) – to the second one. The maps confirm that in the both intervals the ULF pulsations were most intense in the morning. In the first case the strongest ULF waves were observed at latitudes of 65°– 72°, which corresponded to our definition of auroral and polar zones. In the second case the ULF enhancement was at 59°–68°. We constructed the maps of the ULF activity distribution in the main phase of this storm when the maximal values of the ULF-index were obtained.

MIDNIGHT  NOON The magnetograms from several auroral stations (MEA, NAQ, and LRV), located at different longitudes, shows the strong ULF wave in the local geomagnetic morning in both intervals: UT (NAQ and LRV) and UT (MEA). Morning ULF pulsations are registered near the substorm maximum.

Strong Stroms Moderate Storms We compare the variations in the ULF index in the auroral zone during strong magnetic storms with Dstmin varying from –100 to –150 nT and moderate storms with Dstmin varying from –50 to –100 nT. The general regularities in the geomagnetic pulsation variations during strong and moderate storms are similar and differ in only the level of amplitudes.

CONCLUSION We upgraded the base version of ULF-index and applied it to Pc5/Pi3 pulsations study in different MLT sectors and different ranges of geomagnetic latitudes during the different phases of strong magnetic storms. It was found: We upgraded the base version of ULF-index and applied it to Pc5/Pi3 pulsations study in different MLT sectors and different ranges of geomagnetic latitudes during the different phases of strong magnetic storms. It was found: In polar latitudes the greatest ULF activity is observed in the morning sector in all phases of magnetic storms. In polar latitudes the greatest ULF activity is observed in the morning sector in all phases of magnetic storms. In auroral latitudes the ULF-index demonstrates a strong maximum in the morning in the main phases of magnetic storms. In the initial and recovery phases, the morning ULF activity (Pc5) is comparable with the night ULF activity (Pi3). In auroral latitudes the ULF-index demonstrates a strong maximum in the morning in the main phases of magnetic storms. In the initial and recovery phases, the morning ULF activity (Pc5) is comparable with the night ULF activity (Pi3). In subauroral latitudes the enhancement of night-side ULF activity could be a result of the auroral magnetic activity shifting to lower latitudes during the development of the storm main phase. In subauroral latitudes the enhancement of night-side ULF activity could be a result of the auroral magnetic activity shifting to lower latitudes during the development of the storm main phase.

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