In this dissertation, we have investigated the structure and dynamics of small-scale magnetic bright points (MBPs) in quiet, internetwork regions of the lower solar atmosphere. Such BMPs are associated with small-scale, intense (generally kG) magnetic elements. We used high spatial and temporal resolution observations, obtained by the Sunrise baloon-borne solar observatory, to particularly adress (1) observational properties of isolated internetwork Ca II H MBPs, (2) migration of Ca II H MBPs in the internetwork areas, (3) propagation of high-frequency fast waves in small magnetic elements in the lower solar atmosphere, and (4) distribution of magnetic field’s inclination in small quiet-Sun magnetic features. The results of these studies have implications for, e. g., our understanding of the heating mechanisms in the higher layers of the solar atmosphere, estimates of the solar magnetic flux as well as the structure of the convection flows (within a supergranule) advecting small magnetic elements.
Achat du livre
Dynamics of magnetic bright points in the lower solar atmosphere, Shahin Jafarzadeh
Langue
Année de publication
2013
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In this dissertation, we have investigated the structure and dynamics of small-scale magnetic bright points (MBPs) in quiet, internetwork regions of the lower solar atmosphere. Such BMPs are associated with small-scale, intense (generally kG) magnetic elements. We used high spatial and temporal resolution observations, obtained by the Sunrise baloon-borne solar observatory, to particularly adress (1) observational properties of isolated internetwork Ca II H MBPs, (2) migration of Ca II H MBPs in the internetwork areas, (3) propagation of high-frequency fast waves in small magnetic elements in the lower solar atmosphere, and (4) distribution of magnetic field’s inclination in small quiet-Sun magnetic features. The results of these studies have implications for, e. g., our understanding of the heating mechanisms in the higher layers of the solar atmosphere, estimates of the solar magnetic flux as well as the structure of the convection flows (within a supergranule) advecting small magnetic elements.
