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Bazilevskaya G. A. Daibog E. I. Logachev Yu. I. Vlasova N. A. Ginzburg E. A. Ishkov V. N. Lazutin L. L. Nguyen M. D. Surova G. M. Yakovchouk O. S. 《Geomagnetism and Aeronomy》2021,61(1):6-13
Geomagnetism and Aeronomy - Homogeneous series of solar cosmic-ray events for four solar-activity cycles against the background of decreased activity in cycles 23 and 24 are considered. The number... 相似文献
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I. S. Veselovsky K. Mursula N. G. Ptitsyna M. I. Tyasto O. S. Yakovchouk 《Geomagnetism and Aeronomy》2009,49(2):163-168
Based on an analysis of the available archived data from the Russian network of geomagnetic stations, it has been indicated that the known event of August–September 1859 was the first and the greatest event in the series of the recurrent geomagnetic storms. Similar series were repeatedly observed in the next years. These series are caused by the processes on the Sun and in the heliosphere related to the superposition of the solar wind flows. The sporadic and regular components in joint activity of the complex, including active regions and coronal holes on the rotating Sun, play the role of the Bartels M regions responsible for initiation and development of geomagnetic storms. Neither coronal holes nor active regions can separately explain observations. During interpretation, active regions and coronal holes should be considered as a unified complex. 相似文献
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I. N. Myagkova Yu. S. Shugay I. S. Veselovsky O. S. Yakovchouk 《Solar System Research》2013,47(2):127-140
This paper analyzes variations of flux of relativistic and subrelativistic electrons in the outer radiation belt of the Earth caused by the arrival of recurrent high-speed streams of solar wind during three consecutive solar rotations. The period from April to July 2010 is covered. During this time, an increase in fluxes of relativistic electrons was observed after they had reached a minimum in November 2009–January 2010. Two coronal holes of different polarity, geometry, and location relative to the solar equator were the source of high-speed solar wind streams. The relationship between the efficiency of acceleration of electrons of subrelativistic energies and the amplitude, duration of high-speed streams of solar wind and geomagnetic disturbances, as well as the wave activity in the range of 2–7 mHz, characterized by the ULF index, is confirmed. Significant increases of the flux of relativistic electrons in the outer radiation belt of the Earth were observed during the considered period with an hourly average speed of solar wind streams above 550 km/s and a duration of more than seven days. It is found that the spectrum of electrons in the Earth’s outer radiation belt over the considered period of time was softer during the observation of solar wind streams from the positive polarity coronal hole, even given the amplitude of the solar wind velocity higher than 550 km/s. 相似文献
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M. I. Tyasto N. G. Ptitsyna I. S. Veselovsky O. S. Yakovchouk 《Geomagnetism and Aeronomy》2009,49(2):153-162
A retrospective analysis of the Russian magnetic observations of the Carrington event that occurred on September 2–3, 1859, has been performed. The conclusion has been made that this event was caused by the series of three recurrent eruptive solar flares during ～40 h. The characteristics of the geomagnetic crochet, related to a considerable flux of the ionizing electromagnetic radiation during this flare, have been studied. The value and direction of a magnetic field disturbance, registered during the maximum of the geomagnetic storm of September 2, unambiguously indicate that all Russian stations were in the auroral oval zone, which was strongly expanded southward from its average position. The disturbance dependence on the station longitude—the absence of magnetometer pinning in Nerchinsk—is interpreted as the possible manifestation of a strong asymmetry in the effective contour of the current system, which was connected to the heliosphere and covered the disturbed magnetosphere and ionosphere during the short period that lasted only 1–3 h. 相似文献
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The proton energy spectra I(E, t) as functions of time were obtained and analyzed in the energy range of a few tens of MeV on the basis of GOES observations of proton enhancements during solar cycle 23. The energy spectra were approximated by power-law functions. We found a wide variety of functions I(E, t) for studied events. The spectra cannot be described by a universal function of time, although three groups of proton events seem to have some common features. This allows us to outline an approach to their empirical classification in future using a number of dimensionless scaling parameters. The regularities we observe may be partly due to the dynamical processes occurring on the Sun, in the heliosphere, and magnetosphere. 相似文献
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Yu. S. Shugay I. S. Veselovsky O. S. Yakovchouk I. N. Myagkova 《Geomagnetism and Aeronomy》2014,54(5):558-567
The relativistic electron flux in the Earth’s outer radiation belt generally decreased by almost three orders of magnitude during the minimum of cycle 23 in 2009. Such a behavior was possibly caused by very low geomagnetic activity during an extremely weak interplanetary field in that period. This decrease was replaced by an increase in the relativistic electron flux by two orders of magnitude during several months after the sunspot minimum at the beginning of 2010. 相似文献
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Solar and Heliospheric Causes of Geomagnetic Perturbations during the Growth Phase of Solar Cycle 23
Bothmer V. Veselovsky I. S. Dmitriev A. V. Zhukov A. N. Cargill P. Romashets E. P. Yakovchouk O. S. 《Solar System Research》2002,36(6):499-506
A database is compiled for the study of solar and heliospheric causes of geomagnetic perturbations with the daily average index A
> 20 that were observed in the period 1997–2000. The number of such events (more than 200) progressively increased and fluctuated as the current solar cycle developed. It is established that geomagnetic storms are generated by dynamical processes and structures near the center of the solar disk in a zone of several tens of degrees, and these processes are responsible for the appearance in the Earth's region, within several tens of hours, of quasistationary and transient solar wind streams with a sufficiently strong southward component of the heliospheric magnetic field. These streams lasted more than a few hours. The following structures can serve as morphological indicators for the prediction of the appearance of such streams: (1) active and disappearing filaments derived from synoptic -maps of the Sun, (2) solar flares, (3) coronal holes and evolving active regions, and (4) the heliospheric current sheet. The geometry of coronal mass ejections needs further observational study. 相似文献
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