2013/08/01 by J. Warnecke, Jörn Warnecke, Axel Brandenburg · 1 citation
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astrophysics #Context (archaeology) #Convection #Convection zone #Corona (planetary geology) #Coronal hole #Coronal loop #Coronal mass ejection #Coronal plane #Dynamo #Dynamo theory #Geology #Geomagnetism and Paleomagnetism Studies #Magnetic field #Magnetic helicity #Magnetohydrodynamics #Mechanics #Physics #Solar and Space Plasma Dynamics #Solar dynamo #Solar wind #astro-ph.SR
paper · pdf · doi:10.1017/s1743921314001884
published as Magnetic fields throughout stellar evolution, ed. M. Jardine, Proc. IAU Symp., Vol. 302, pp. 134-137 (2014) · 4 pages, 1 figure, To appear in proceedings of IAUS 302: Magnetic fields throughout stellar evolution (August 2013, Biarritz, France)
openalex publication_date 2013/08/01 · arxiv created 2013/10/02 · arxiv updated 2014/09/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We report on turbulent dynamo simulations in a spherical wedge with an outer coronal layer. We apply a two-layer model where the lower layer represents the convection zone and the upper layer the solar corona. This setup is used to study the coronal influence on the dynamo action beneath the surface. Increasing the radial coronal extent gradually to three times the solar radius and changing the magnetic Reynolds number, we find that dynamo action benefits from the additional coronal extent in terms of higher magnetic energy in the saturated stage. The flux of magnetic helicity can play an important role in this context.