2011/06/05 by Rui F. Pinto, Allan Sacha Brun, Laurène Jouve +1 · 2 citations
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Angular momentum #Astro and Planetary Science #Coupling (piping) #Dynamo #Geomagnetism and Paleomagnetism Studies #Momentum (technical analysis) #Solar and Space Plasma Dynamics #Solar dynamo #Solar wind #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/737/2/72
arxiv created 2011/06/05 · openalex publication_date 2011/08/04 · arxiv updated 2015/05/28 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We study the connections between the Sun's convection zone and the evolution of the solar wind and corona. We let the magnetic fields generated by a 2.5-dimensional (2.5D) axisymmetric kinematic dynamo code (STELEM) evolve in a 2.5D axisymmetric coronal isothermal magnetohydrodynamic code (DIP). The computations cover an 11 year activity cycle. The solar wind's asymptotic velocity varies in latitude and in time in good agreement with the available observations. The magnetic polarity reversal happens at different paces at different coronal heights. Overall the Sun's mass-loss rate, momentum flux, and magnetic braking torque vary considerably throughout the cycle. This cyclic modulation is determined by the latitudinal distribution of the sources of open flux and solar wind and the geometry of the Alfvén surface. Wind sources and braking torque application zones also vary accordingly.