Comparative analysis of recurrent high-speed solar wind streams influence on the radiation environment of near-earth space in April–July 20101
| Autor: | Irina Myagkova, O. S. Yakovchouk, Igor Veselovsky, Yu. S. Shugay |
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| Rok vydání: | 2013 |
| Předmět: |
Solar minimum
Physics Astrophysics::High Energy Astrophysical Phenomena Coronal hole Astronomy and Astrophysics Solar cycle 22 Atmospheric sciences Solar maximum Corona Polar wind Space and Planetary Science Physics::Space Physics Coronal mass ejection Astrophysics::Solar and Stellar Astrophysics Magnetopause Astrophysics::Earth and Planetary Astrophysics |
| Zdroj: | Solar System Research. 47:127-140 |
| ISSN: | 1608-3423 0038-0946 |
| DOI: | 10.1134/s0038094613020068 |
| Popis: | 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. |
| Databáze: | OpenAIRE |
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