Together, these two facts prompt the general question: whether the solar dynamo is possiblya near-surface instability. Here we report strong affirmative evidence in stark contrast to traditional modelsfocusing on the deeper tachocline. Simple analytic estimates show that the near-surface magneto-...
A number of problems of solar and stellar dynamo theory are briefly reviewed and the current status of possible solutions is discussed. Results of direct numerical simulations are described in view of mean-field dynamo theory and the relation between the alpha-effect and the inverse cascade of mag...
we used two three-dimensional models of the solar photosphere taken from a magneto-convection simulation with small-scale dynamo action, one virtually unmagnetized, and the other characterized by a mean field strength of 160 G in the low photosphere. We performed local thermodynamic equilibrium spe...
The solar surface dynamo has become an active area of research in an attempt to understand the origin of a variety of magnetic field structures on the sun. The major modification that needs to be incorporated in the standard dynamo process is the inclusion of the partial ionization of the gas...
The solar dynamo is the process by which the Sun's magnetic field is generated through the interaction of the field with convection and rotation. In this, it is kin to planetary dynamos and other stellar dynamos. Although the precise mechanism by which the Sun generates its field remains ...
Context. Observations indicate that the 'quiet ' solar photosphere outside active regions contains considerable amounts of magnetic energy and magnetic flux, with mixed polarity on small scales. The origin of this flux is unclear. Aims. We test whether local dynamo action of the near-surface con...
We propose a self-consistent explanation of Rieger-type periodicities, the Schwabe cycle, and the Suess-de Vries cycle of the solar dynamo in terms of resonances of various wave phenomena with gravitational forces exerted by the orbiting planets. Starting on the high-frequency side, we show that...
It is shown that the power ε generated by the solar wind-magnetosphere dynamo is transmitted to the convective motion of magnetospheric plasma. This convective motion generates what we may call the "Pedersen counterpart currents" in the magnetosphere and drives a large part of the "region 1 and...
2.2 What is the three-dimensional structure of convection and circulation flows below the surface, and how does it affect solar activity? This objective addresses directly one of the fundamental questions in solar physics: How and where does the solar dynamo operate, and in what way do the fiel...
arXiv:1504.07835v3 [astro-ph.SR] 2 Sep 2015Dynamo Ef f ects Near Transition from Solar to Anti-SolarDif f erential RotationRadostin D. Simitev 1,2,3 , Alexander G. Kosovichev 3,4 , and Friedrich H. Busse 2,5Received ; accepted1 School of Mathematics and Statistics, University of ...