|
ИСТИНА |
Войти в систему Регистрация |
ФНКЦ РР |
||
Clarifying physical properties of magnetic fields in sunspotsтезисы доклада
- Авторы: Obridko V., Sokoloff D., Livshits I., Shelting B., Katsova M.
- Сборник: 44th COSPAR Scientific Assembly
- Тезисы
- Год издания: 2022
- Место издания: COSPAR Athena
- Номер статьи: D1.2-0057-22
- Аннотация: From the very beginning and long afterwards, the number and area of sunspots were determined visually from solar images based on their photometric properties. Nowadays, we are using photo and numerical records. There is no doubt, however, that the main factor determining the very existence of a sunspot is the magnetic field. Nevertheless, a definition of the sunspot boundary in terms of the magnetic field is still absent in scientific literature. Here, we suggest such a definition based on SDO/HMI observations. We demonstrate that the radial magnetic field component at the outer boundary of the penumbra is about 550 Mx/cm2 independent of the sunspot area and the maximum magnetic field in the umbra. The mean magnetic field intensity in sunspots grows slightly as the sunspot area increases up to 500-1000 m.v.h. and may reach about 900 Mx/cm2 . The mean field in umbrae is around 2000 Mx/cm2 The total magnetic flux weakly depends on the maximum field strength in a sunspot and is determined by the spottedness, i.e., the sunspot number and the total sunspot area; however, the relation between the total flux and the sunspot area is substantially nonlinear. We suggest an explicit parametrization for this relation. The contribution of the magnetic flux associated with sunspots to the total magnetic flux is small, not achieving more than 20% even at the maximum of the solar activity. Acknowledgements VNO, MMK, DDS acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780.
- Добавил в систему: Соколов Дмитрий Дмитриевич