Simulations of solar wind variations during an 11-year cycle and the influence of north-south asymmetry

Abstract

We want to study the connections between the magnetic field generated inside the Sun and the solar wind impacting Earth, especially the influence of north-south asymmetry on the magnetic and velocity fields. We study a solar-like 11-year cycle in a quasi-static way: an asymmetric dynamo field is generated through a 2.5-dimensional (2.5-D) flux-transport model with the Babcock-Leighton mechanism, and then is used as bottom boundary condition for compressible 2.5-D simulations of the solar wind. We recover solar values for the mass loss rate, the spin-down time scale and the Alfvén radius, and are able to reproduce the observed delay in latitudinal variations of the wind and the general wind structure observed for the Sun. We show that the phase lag between the energy of the dipole component and the total surface magnetic energy has a strong influence on the amplitude of the variations of global quantities. We show in particular that the magnetic torque variations can be linked to topological variations during a magnetic cycle, while variations in the mass loss rate appear to be driven by variations of the magnetic energy.

arXiv comment27 pages, 11 figures, Space Weather Special Issue

References in corpus (24)

• PLUTO: a Numerical Code for Computational Astrophysics
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence
• Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
• Radiative MHD simulation of sunspot structure
• Making the corona and the fast solar wind: a self-consistent simulation for the low-frequency Alfven waves from photosphere to 0.3AU
• Magnetic Braking Formulation for Sun-Like Stars: Dependence on Dipole Field Strength and Rotation Rate
• The effect of magnetic topology on thermally-driven winds: towards a general formulation of the braking law
• Magnetic Cycles in a Convective Dynamo Simulation of a Young Solar-type Star
• The Open Flux Problem
• Twisted flux tube emergence from the convection zone to the corona
• Solar Magnetic Field Reversals and the Role of Dynamo Families
• Grand Minima and Equatorward Propagation in a Cycling Stellar Convective Dynamo
• On the role of meridional flows in flux transport dynamo models
• Asymmetric Solar Polar Field Reversals
• Coupling from the photosphere to the chromosphere and the corona
• Connecting the Sun and the Solar Wind: The First 2.5 Dimensional Self-consistent MHD Simulation under the Alfvén Wave Scenario
• Coupling the solar dynamo and the corona: wind properties, mass and momentum losses during an activity cycle
• Reconciling solar and stellar magnetic cycles with nonlinear dynamo simulations
• Seismic tests for solar models with tachocline mixing
• Reconstruction of Helio-latitudinal Structure of the Solar Wind Proton Speed and Density
• Global solar magnetic field organization in the outer corona: influence on the solar wind speed and mass flux over the cycle
• Simulation Study of Hemispheric Phase-Asymmetry in the Solar Cycle
• Variational estimation of the large scale time dependent meridional circulation in the Sun: proofs of concept with a solar mean field dynamo model
• Production of sunspots and their effects on the corona and solar wind: Insights from a new 3D flux-transport dynamo model

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