3D MHD Modeling of the Impact of Subsurface Stratification on the Solar Dynamo

Abstract

Various models of solar subsurface stratification are tested in the global EULAG-MHD solver to simulate diverse regimes of near-surface convective transport. Sub- and superadiabacity are altered at the surface of the model ($r>0.95R_{\odot }$) to either suppress or enhance convective flow speeds in an effort to investigate the impact of the near-surface layer on global dynamics. A major consequence of increasing surface convection rates appears to be a significant alteration of the distribution of angular momentum, especially below the tachocline where the rotational frequency predominantly increases at higher latitudes. These hydrodynamic changes correspond to large shifts in the development of the current helicity in this stable layer ($r<0.72R_{\odot }$), significantly altering its impact on the generation of poloidal and toroidal fields at the tachocline and below, acting as a major contributor towards transitions in the dynamo cycle. The enhanced near-surface flow speed manifests in a global shift of the toroidal field ($B_{\varphi }$) in the butterfly diagram - from a North-South symmetric pattern to a staggered anti-symmetric emergence.

References in corpus (6)

• Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
• The case for a distributed solar dynamo shaped by near-surface shear
• Meridional Circulation in Solar and Stellar Convection Zones
• Turbulent magnetic pumping in a Babcock-Leighton solar dynamo model
• The radial gradient of the near-surface shear layer of the Sun
• Quenching and anisotropy of hydromagnetic turbulent transport

Cited by in corpus (3)

• Redundant-Baseline Calibration of the Hydrogen Epoch of Reionization Array
• Leptocline as a Shallow Substructure of Near-Surface Shear Layer in 3D Radiative Hydrodynamic Simulations
• Constraining Global Solar Models through Helioseismic Analysis