Magnetic fine structure in the solar photosphere

Autor*innen

• Sanja Danilović

Parameter

• Lehrbücher
• Universitätslehrbücher

Mehr zum Buch

The fine structure of the magnetic field in the solar photosphere arises from complex interactions between the magnetic field and convection. Despite significant improvements in spatial resolution of observational instruments, many magnetic features remain unresolved, even with the highest resolution available. Realistic magnetohydrodynamic (MHD) numerical models of solar surface layers now offer a level of realism and accuracy that allows for quantitative comparisons with observational data. These simulations serve as valuable tools for analyzing and interpreting observations, providing insights into the intricate interactions between magnetic fields and convection at scales and depths that are not accessible through direct observation. This research synthesizes spectropolarimetric signals from 3D radiative MHD simulations and compares them with data from the Hinode satellite's Spectropolarimeter. A theoretical Point Spread Function is developed to account for instrumental effects. The study addresses characteristics of granulation and internetwork magnetic fields, showcasing examples of formation and cancellation of magnetic concentrations in simulations. It also explores potential observational signatures of these processes, the impacts of spatial smearing, and discusses the role of the surface dynamo in quiet Sun magnetism, estimating the magnetic flux within the internetwork.

• Sprache: Englisch
• Erscheinungsdatum: 2010
• Einband: Paperback