F Stefani, A Giesecke, T Weier - Solar Physics, 2019 - Springer
We discuss a solar dynamo model of Tayler–Spruit type whose Ω Ω-effect is conventionally produced by a solar-like differential rotation but whose α α-effect is assumed to be …
ДД Соколов, РА Степанов, ПГ Фрик - Успехи физических наук, 2014 - ufn.ru
Вопрос о возникновении и последующей эволюции магнитных полей небесных тел, составляющий предмет теории динамо, интересовал ЯБ Зельдовича многие годы. За …
F Stefani, A Giesecke, N Weber, T Weier - Solar Physics, 2016 - Springer
Recent years have seen an increased interest in the question of whether the gravitational action of planets could have an influence on the solar dynamo. Without discussing the …
V Kumar, F Pizzi, A Giesecke, J Šimkanin… - Physics of …, 2023 - pubs.aip.org
The effect of the nutation angle on the flow inside a precessing cylinder is experimentally explored and compared with numerical simulations. The focus is laid on the typical …
The Tayler instability is a kink-type, current driven instability that plays an important role in plasma physics but might also be relevant in liquid metal applications with high electrical …
A Giesecke, T Vogt, F Pizzi, V Kumar… - Journal of Fluid …, 2024 - cambridge.org
We examine the fluid flow forced by precession of a rotating cylindrical container using numerical simulations and experimental flow measurements with ultrasonic Doppler …
F Stefani, A Giesecke, N Weber, T Weier - Solar Physics, 2018 - Springer
The solar cycle appears to be remarkably synchronized with the gravitational torques exerted by the tidally dominant planets Venus, Earth and Jupiter. Recently, a possible …
F Pizzi, A Giesecke, J Simkanin, V Kumar… - arXiv preprint arXiv …, 2023 - arxiv.org
The upcoming DRESDYN (DREsden Sodium facility for DYNnamo and thermohydraulic studies) precession experiment will test the possibility to achieve magnetohydrodynamic …
The existence of energy cascades as signatures of conserved magnitudes is one of the universal characteristics of turbulent flows. In homogeneous 3D turbulence, the energy …