Three-dimensional magnetohydrodynamic simulation of the solar magnetic flux emergence: Parametric study on the horizontal divergent flow

Abstract

Solar active regions are formed through the emergence of magnetic flux from the deeper convection zone. Recent satellite observations have shown that a horizontal divergent flow (HDF) stretches out over the solar surface just before the magnetic flux appearance. The aims of this study are to investigate the driver of the HDF and to see the dependency of the HDF on the parameters of the magnetic flux in the convection zone. We conduct three-dimensional magnetohydrodynamic (3D MHD) numerical simulations of the magnetic flux emergence and vary the parameters in the initial conditions. An analytical approach is also taken to explain the dependency. The horizontal gas pressure gradient is found to be the main driver of the HDF. The maximum HDF speed shows positive correlations with the field strength and twist intensity. The HDF duration has a weak relation with the twist, while it shows negative dependency on the field strength only in the case of the stronger field regime. Parametric dependencies analyzed in this study may allow us to probe the structure of the subsurface magnetic flux by observing properties of the HDF.

7 pages, 5 figures, 1 table, accepted for publication in Astronomy & Astrophysics

References in corpus (3)

• Numerical Experiments on the Two-step Emergence of Twisted Magnetic Flux Tubes in the Sun
• Detection of the Horizontal Divergent Flow prior to the Solar Flux Emergence
• Large-scale 3D MHD simulation on the solar flux emergence and the small-scale dynamic features in an active region

Cited by in corpus (10)

• Formation of a Flare-Productive Active Region: Observation and Numerical Simulation of NOAA AR 11158
• Statistical Analysis of the Horizontal Divergent Flow in Emerging Solar Active Regions
• The emergence of magnetic flux and its role on the onset of solar dynamic events
• Extended statistical analysis of emerging solar active regions
• The origin and early evolution of a bipolar magnetic region in the solar photosphere
• Plasma flows and magnetic field interplay during the formation of a pore
• Successful and Failed Flux Tube Emergence in the Solar Interior
• Photospheric Velocity Structures during the Emergence of Small Active Regions on the Sun
• Morphological study of penumbral formation
• Pre-emergence Signatures Of Horizontal Divergent Flows In Solar Active Regions