2014/09/30 by J. Warnecke, Jörn Warnecke, Petri J. Käpylä +4 · 5 citations
Biochemistry, Genetics and Molecular Biology · Earth and Planetary Sciences · Mathematics · Physics and Astronomy · #Astrophysics #Classical mechanics #Convection #Dynamo #Dynamo theory #Geology #Geomagnetism and Paleomagnetism Studies #Geometry #Geophysics #Geophysics and Gravity Measurements #Magnetic field #Mathematics #Mechanics #Physics #Shear (geology) #Solar and Space Plasma Dynamics #Solar dynamo #Tangent #astro-ph.SR
paper · pdf · doi:10.1088/2041-8205/796/1/l12
published as Astrophys. J. Lett. 796, L12 (2014) · 6 pages, 5 figures, published in ApJ Letters
openalex publication_date 2014/11/05 · arxiv created 2014/11/28 · arxiv updated 2014/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present results from four convectively driven stellar dynamo simulations in spherical wedge geometry. All of these simulations produce cyclic and migrating mean magnetic fields. Through detailed comparisons, we show that the migration direction can be explained by an αΩ dynamo wave following the Parker–Yoshimura rule. We conclude that the equatorward migration in this and previous work is due to a positive (negative) α effect in the northern (southern) hemisphere and a negative radial gradient of Ω outside the inner tangent cylinder of these models. This idea is supported by a strong correlation between negative radial shear and toroidal field strength in the region of equatorward propagation.