Momentum transport in fusion and astrophysical systems

Momentum transport impacts the development of transport barriers and intrinsic rotation in MFE plasmas, is critical to accretion disks, and to the formation of the solar tachocline (a thin sheared rotation layer at the base of the solar convection zone), which is thought to then play a critical role in the solar dynamo and formation of solar flares. Presentations from fusion and laboratory plasma devices, hydrodynamic experiments, basic theory, and numerical simulations with fluid and gyrokinetic approaches are planned.

Format: oral presentations

Organizers: George Tynan and Pat Diamond, on behalf of the Center for Momentum Transport and Flow Organization.

Integrated, Multiphysics, High‑Performance Computations for Magnetic Fusion Research

With the rise in cost associated with experimental physics, integrated multiphysics, high-performance computations are increasingly important for prediction and analysis. These computations take advantage of leadership class computational hardware while bringing in models for differing physics (e.g., MHD and RF or plasma and neutrals), different regions (e.g., core and edge), different dynamics (axisymmetric transport versus nonaxisymmetric relaxation events), or other. Producing accurate multiphysics computations is interdisciplinary, requiring teams that involve plasma physicists, applied mathematicians, and computer scientists. Speakers from these multiple disciplines will present the latest methods for and results from integrated multiphysics, high‑performance computations.

Format: oral and poster presentations

Organizers: Scott Kruger, Lee Berry, Harold Weitzner.

Solar wind turbulence: Theoretical and Observational Perspectives

The solar wind is an excellent in‑situ laboratory for investigating nonlinear and turbulent processes in a magnetized plasma fluid since it comprises a multitude of spatial and temporal length-scales associated with an admixture of waves, fluctuations, structures and nonlinear turbulent interactions. Although the dynamical evolution of multiple scales leads to a complex picture, it also provides an opportunity to test the validity of various existing wave, nonlinear structures and turbulence theories. For instance, low frequency solar wind fluctuations are described typically by an MHD description of plasma that is characterized typically by a Kolmogorov‑like spectrum. The power spectrum is observed frequently, both in the interstellar medium and solar wind. This scaling breaks down above the ion cyclotron frequency and exhibits a steeper power law. The evolution of the spectrum on a variety of length scales is one of the long standing puzzles of classical statistical theories of turbulence, with implications for transport, cosmic rays, and energetic particles. This mini-conference focuses on underpinning these complex nonlinear processes that mediate solar wind turbulence from theoretical, modeling and observational perspectives.

Format: oral presentations (possibly some posters)

Organizers: Dastgeer Shaikh and G.P. Zank.

Electromagnetic metamaterials for high‑power applications

Metamaterials promise to revolutionize the way high power microwaves are generated and/or applied. However, very little is known about their response to high‑power microwaves. A variety of high-field phenomena such as breakdown, anomalous absorption, pulsed heating, etc. could strongly influence their performance. These issues will be addressed by experts in particle acceleration, high-power microwave generation, metamaterials design, and the physics of breakdown.

Format: oral presentations

Organizers: Gennady Shvets, Y.Y. Lau, Edl Schamiloglu.