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Solar sources and characteristics of solar wind magnetic cloudsстатья Исследовательская статья
- Авторы: Barkhatov N.А., Revunova Е.А., Romanov R.V., Vorobjev V.G.
- Журнал: Physics of Auroral Phenomena
- Год издания: 2018
- Издательство: Федеральное государственное бюджетное научное учреждение "Полярный геофизический институт"
- Местоположение издательства: Апатиты
- Первая страница: 66
- Последняя страница: 68
- DOI: 10.25702/KSC.2588-0039.2018.41.66-68
- Аннотация: The forecast quality for geomagnetic efficiency of coronal mass ejections (CME) as high-energy solar manifestations in the form of magnetic clouds directly depends on the initial physical characteristics of solar sources [1, 2, 3]. For this purpose, at the present study a technique for establishing the localization and orientation of an extended solar source of magnetic clouds from the data of coronagraphs and photosphere photographs EIT MDI SOHO has developed. Further, based on the proposed method, a statistical study of the dependences for CMEs spatial characteristics of magnetic clouds on the location of their sources on the solar disk, on their extent and angular orientation was performed. As a result, dependences of the maximum intensity, of the maximum intensity Bz-component, the latitude and longitude angles of the cloud magnetic field vector, the magnetic cloud velocity from the minimum latitude of the extended solar source and the corresponding longitude are obtained. Attention has been drawn to the existence of auroral electrojets AL index value dependence by parameters of solar sources structures. The relationships of solar source coordinates with the geomagnetic activity of the cloud sheath and with the geomagnetic activity of the magnetic cloud body are found. The main problems in studying the sources of CME/MC and their transfer in the solar wind are the following: 1) the CMEs sources often do not stand out against the background of the corona or the photosphere and sometimes can be determined by residual phenomena; 2) solitary MC is an extremely rare phenomenon and its source is difficult to detect against the background of a disturbed solar corona or photosphere, 3) the direct passage of solitary MC to the Earth is not fixed by coronagraphs, since the coronagraph detects the MC only in the profile, 4) the huge dimensions of the CME/MC by satellites allows to receive the parameters of the structure and its dynamics only at the object section.
- Добавил в систему: Воробьев Вячеслав Георгиевич