Complex Magnetic Evolution and Magnetic Helicity in the Solar Atmosphere

Abstract

Solar atmosphere is a single system unified by the presence of large-scale magnetic fields. Topological changes in magnetic fields that occur in one place may have consequences for coronal heating and eruptions for other, even remote locations. Coronal magnetic fields also play role in transport of magnetic helicity from Sun's subphotosphere/upper convection zone to the interplanetary space. We discuss observational evidence pertinent to some aspects of the solar corona being a global interconnected system, i.e., large-scale coronal heating due to new flux emergence, eruption of chromospheric filament resulting from changes in magnetic topology triggered by new flux emergence, sunspots rotation as manifestation of transport of helicity through the photosphere, and potential consequences of re-distribution of energy from solar luminosity to the dynamo for solar cycle variations of solar irradiance.

9 pages, 3 figures

References in corpus (2)

• Jets in coronal holes: Hinode observations and 3D computer modelling
• Magnetic Connectivity between Active Regions 10987, 10988, and 10989 by Means of Nonlinear Force-Free Field Extrapolation

Cited by in corpus (4)

• Studying the transfer of magnetic helicity in solar active regions with the connectivity-based helicity flux density method
• Search for a Signature of Twist-Removal in the Magnetic Field of Sunspots in Relation with Major Flares
• Solar radius and luminosity variations induced by the internal dynamo magnetic fields
• Magnetic bipoles in rotating turbulence with coronal envelope