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Origin and Ion Charge State Evolution of Solar Wind Transients during 4 – 7 August 2011статья
Информация о цитировании статьи получена из
Web of Science,
Scopus
Статья опубликована в журнале из списка Web of Science и/или Scopus
Дата последнего поиска статьи во внешних источниках: 7 сентября 2017 г.
- Авторы: Rodkin D., Goryaev F., Pagano P., Gibb G., Slemzin V., Shugay Yu, Veselovsky I., Mackay D.H.
- Журнал: Solar Physics
- Том: 292
- Номер: 7
- Год издания: 2017
- Издательство: Springer Netherlands
- Местоположение издательства: Dordrecht, Netherlands
- Первая страница: 90
- DOI: 10.1007/s11207-017-1109-0
- Аннотация: We present a study of the complex event consisting of several solar wind tran-sients detected by the Advanced Composition Explorer (ACE) on 4 – 7 August 2011, whichcaused a geomagnetic storm with Dst = −110 nT. The supposed coronal sources, threeflares and coronal mass ejections (CMEs), occurred on 2 – 4 August 2011 in active region(AR) 11261. To investigate the solar origin and formation of these transients, we study thekinematic and thermodynamic properties of the expanding coronal structures using the SolarDynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) EUV images and differential emission measure (DEM) diagnostics. The Helioseismic and Magnetic Imager (HMI)magnetic field maps were used as the input data for the 3D magnetohydrodynamic (MHD)model to describe the flux rope ejection (Pagano, Mackay, and Poedts, 2013b). We character-ize the early phase of the flux rope ejection in the corona, where the usual three-componentCME structure formed. The flux rope was ejected with a speed of about 200 km s−1to theheight of 0.25 R. The kinematics of the modeled CME front agrees well with the SolarTerrestrial Relations Observatory (STEREO) EUV measurements. Using the results of theplasma diagnostics and MHD modeling, we calculate the ion charge ratios of carbon andoxygen as well as the mean charge state of iron ions of the 2 August 2011 CME, takinginto account the processes of heating, cooling, expansion, ionization, and recombination ofthe moving plasma in the corona up to the frozen-in region. We estimate a probable heat-ing rate of the CME plasma in the low corona by matching the calculated ion compositionparameters of the CME with those measured in situ for the solar wind transients. We alsoconsider the similarities and discrepancies between the results of the MHD simulation andthe observations.
- Добавил в систему: Шугай Юлия Сергеевна