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Physics Design for ARIES-CS

L. P. Ku, P. R. Garabedian, J. Lyon, A. Turnbull, A. Grossman, T. K. Mau, M. Zarnstorff, ARIES Team

Fusion Science and Technology / Volume 54 / Number 3 / October 2008 / Pages 673-693

Technical Paper / Aries-Cs Special Issue

Novel stellarator configurations have been developed for ARIES-CS. These configurations are optimized to provide good plasma confinement and flux surface integrity at high beta. Modular coils have been designed for them in which the space needed for the breeding blanket and radiation shielding was specifically targeted such that reactors generating GW electrical powers would require only moderate major radii (<10 m). These configurations are quasi-axially symmetric in the magnetic field topology and have small numbers of field periods (3) and low aspect ratios (6). The baseline design chosen for detailed systems and power plant studies has three field periods, aspect ratio 4.5, and major radius 7.5 m operating at ~ 6.5% to yield 1 GW of electric power. The shaping of the plasma accounts for 75% of the rotational transform. The effective helical ripples are very small (<0.6% everywhere), and the energy loss of alpha particles is calculated to be 5% when operating in high-density regimes. An interesting feature in this configuration is that instead of minimizing all residues in the magnetic spectrum, we preferentially retained a small amount of the nonaxisymmetric mirror field. The presence of this mirror and its associated helical field alters the ripple distribution, resulting in the reduced ripple-trapped loss of alpha particles despite the long connection length in a tokamak-like field structure. Additionally, we discuss two other potentially attractive classes of configurations, both quasi-axisymmetric: one with only two field periods, very low aspect ratios (~2.5), and less complex coils, and the other with the plasma shaping designed to produce low-shear rotational transform so as to ensure the robustness and integrity of flux surfaces when operating at high .

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