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MAGNETIC FIELD STRUCTURE AND SOLAR WIND STREAMS NEAR SOLAR MAXIMUM OF 2012тезисы доклада
- Авторы: Shugay Yu S., Slemzin V.A., Veselovsky I.S.
- Сборник: The Sun: active and quiet – 2013, International Workshop on Solar Physics, December 16 – 20, 2013
- Тезисы
- Год издания: 2013
- Место издания: Moscow, LPI
- Первая страница: 32
- Последняя страница: 32
- Аннотация: We consider evolution of the global solar coronal magnetic field, sources of the solar wind and the interplanetary magnetic field sector structure during the period of the polarity reversal in 2012 near the maximum of the unusual and weak 24-rd solar cycle. Using the solar wind data from ACE, EUV images from SDO and Proba-2, as well as ground based WSO magnetic field maps we investigated a correlation between the measured and calculated magnetic fields in the coronal source regions with solar wind velocity and density flux. The results demonstrate a good correspondence between expected and observed four sector structure of interplanetary magnetic field with exceptions due to the solar activity events (coronal mass ejections). The fast solar wind density flux associate with large coronal hole and high-speed sporadic events. The slow solar wind density flux shows the best correlation with total areas of several small coronal holes. An isolated transequatorial coronal hole of the negative polarity were the most notable sources of high speed solar wind streams during February-August 2012. The appearance and disappearance of this coronal hole can be related to the evolution of the global magnetic field. However, the change of the coronal hole boundaries and location may also be influenced by coronal hole differential rotation as well as by the dynamics of surrounding bipolar regions. The geometry of CH boundaries as well as CH area reflect on the SW properties near the Earth’s orbit at that time.
- Добавил в систему: Шугай Юлия Сергеевна