Influence of space weather conditions on the intermittency of the Pi3 irregular geomagnetic pulsations

Мұқаба

Дәйексөз келтіру

Толық мәтін

Ашық рұқсат Ашық рұқсат
Рұқсат жабық Рұқсат берілді
Рұқсат жабық Тек жазылушылар үшін

Аннотация

The influence of substorms intensity, solar wind and interplanetary magnetic field (IMF) parameters on the pattern of amplitude distributions (intermittency) of Pi3 pulsation bursts observed in the night sector of the magnetosphere during substorms development was studied. One-minute digital magnetic field observation data from Arctic and Antarctic observatories were used for the analysis (Heiss Island and Mirny). The index α, which reflects the slope of the cumulative distribution function of the Pi3 burst amplitudes, was considered as the main characteristic of the Pi3 pulsation intermittency. It was shown that the distributions of Pi3 burst amplitudes, depending on space weather conditions, obeyed different power laws. It was found that the α value in the northern and southern hemispheres was greater during the development of weak substorms than during the development of strong and moderate substorms. It was shown that the α values in the two hemispheres were comparable when Pi3 bursts were excited against the background of slow solar wind flows, at the northward direction of the IMF Bz component and at a high level of solar wind plasma turbulence. Under other analyzed conditions, an asymmetry in the change in the α index was found. It is assumed that the intermittency index α qualitatively characterizes the level of plasma turbulence in the region of excitation of Pi3 pulsation bursts.

Толық мәтін

Рұқсат жабық

Авторлар туралы

N. Kurazhkovskaya

Schmidt Institute of Physics of the Earth, Russian Academy of Sciences

Хат алмасуға жауапты Автор.
Email: knady@borok.yar.ru

Borok Geophysical Observatory

Ресей, Borok, Yaroslavl oblast

B. Klain

Schmidt Institute of Physics of the Earth, Russian Academy of Sciences

Email: klain@borok.yar.ru

Borok Geophysical Observatory

Ресей, Borok, Yaroslavl oblast

А. Kurazhkovskii

Schmidt Institute of Physics of the Earth, Russian Academy of Sciences

Email: ksasha@borok.yar.ru

Borok Geophysical Observatory

Ресей, Borok, Yaroslavl oblast

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Жүктеу
2. Fig. 1. Typical examples of observations of Pi3 pulsations (H - component) at the observatories of the island of Heiss (9.11.1997) and Mirny (13.03.1995). Heiss (9.11.1997) and Mirny (13.03.1995). The amplitude spectra of Pi3 pulsations on the interval of their observation are shown on the right. The dynamics of the AL-index is given below.

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3. Fig. 2. Dependence of the observation frequency N of Pi3 pulsations in HIS and MIR on the maximum spectral density of wave packets Smax and its corresponding frequency f.

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4. Fig. 3. Dependence of the observation frequency N of Pi3 pulsations in HIS and MIR on the maximum intensity of substorms characterized by the AE-index value.

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5. Fig. 4. Daily variation of the observation frequency normalized by the maximum number of occurrences N/Nmax of Pi3 pulsations in HIS and MIR.

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6. Fig. 5. Frequency distribution of the occurrence frequency of N Pi3 pulsations in HIS and MIR from large-scale solar wind currents.

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7. Fig. 6. Dependence of the intermittency of Pi3 pulsations in HIS and MIR on the maximum intensity of substorms. On the left are shown the N(A) distributions of Pi3 pulsation burst amplitudes in HIS (black curve) and MIR (gray curve). On the right are the cumulative functions of the CDF distributions of Pi3 pulsation amplitudes in HIS and MIR (dark and light circles, respectively) and their approximation by the degree function (black and gray lines, respectively).

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8. Fig. 7. Dependence of Pi3 pulsation intermittency in HIS and MIR on the velocity of the slow and fast solar wind streams. The notations are the same as in Fig. 6.

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9. Fig. 8.Dependence of Pi3 pulsation intermittency in HIS and MIR on the direction of the Bx-, By-, and Bz-components of the MMP. The designations are the same as in Fig.6.

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10. Fig. 9.Dependence of Pi3 pulsation intermittency in HIS and MIR on the value of the plasma parameter β.The designations are the same as in Fig.6.

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