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Convection and Differential Rotation Properties of G & K Stars Computed with the ASH Code
Sean P. Matt, Olivier Do Cao, B. P. Brown +1
The stellar luminosity and depth of the convective envelope vary rapidly with mass for G- and K-type main sequence stars. In order to understand how these properties influence the…
Buoyant Magnetic Loops in a Global Dynamo Simulation of a Young Sun
Nicholas J. Nelson, Benjamin P. Brown, Allan Sacha Brun +2
The current dynamo paradigm for the Sun and sun-like stars places the generation site for strong toroidal magnetic structures deep in the solar interior. Sunspots and star-spots on…
Global-scale Simulations of Stellar Convection and their Observational Predictions
Benjamin P. Brown
Stars on the lower main sequence (F-type through M-type) have substantial convective envelopes beneath their stellar photospheres. Convection in these regions can couple with rotat…
Numerical simulation of laminar plasma dynamos in a cylindrical von Kármán flow
I. V. Khalzov, B. P. Brown, F. Ebrahimi +2
The results of a numerical study of the magnetic dynamo effect in cylindrical von Kármán plasma flow are presented with parameters relevant to the Madison Plasma Couette Experiment…
Magnetic Cycles in a Convective Dynamo Simulation of a Young Solar-type Star
Benjamin P. Brown, Mark S. Miesch, Matthew K. Browning +2
Young solar-type stars rotate rapidly and many are magnetically active; some undergo magnetic cycles similar to the 22-year solar activity cycle. We conduct simulations of dynamo a…