authors
- CANIK, J.M.
- HIRSHMAN, S.P.
- SANCHEZ FERNANDEZ, LUIS RAUL
- MAINGI, R.
- AHN, J.W.
- BELL, R.E.
- DIALLO, A.
- GERHARDT, S.P.
- LEBLANC, B.P.
- MENARD, J.E.
- PARK, J.K.
- PODESTA, M.
- SABBAGH, S.A.
First use of three-dimensional equilibrium, stability and transport calculations for interpretation of ELM triggering with magnetic perturbations in NSTX
Articles
Overview
published in
- NUCLEAR FUSION Journal
publication date
- May 2012
start page
- 1
end page
- 10
issue
- 5 (54004)
volume
- 52
Digital Object Identifier (DOI)
International Standard Serial Number (ISSN)
- 0029-5515
Electronic International Standard Serial Number (EISSN)
- 1741-4326
abstract
- Conference: 5th International Workshop on Stochasticity in Fusion Plasmas (SFP) Location: Julich, GERMANY Date: APR 11-14, 2011. The application of non-axisymmetric magnetic perturbations has been demonstrated to destabilize edge-localized modes (ELMs) in the National Spherical Torus Experiment. A model 3D equilibrium has been calculated for these experiments using the VMEC code, which assumes nested flux surfaces and therefore that resonant perturbations are shielded. First, a free-boundary equilibrium is calculated using the NSTX coil set, with pressure and current profiles matched to a standard 2D reconstruction, but with up-down symmetry enforced. A new equilibrium is then calculated with the n = 3 field applied at a level consistent with experiment. This equilibrium is then used as the basis of further calculations using codes developed for analysis of stellarator plasmas. The neoclassical transport due to the 3D fields is calculated to be small compared with the experimental transport rates. Initial stability analysis has been performed, and indicates a modest degradation in ballooning stability with 3D fields applied. A new 3D equilibrium is also calculated using the SIESTA code, which allows for the formation of islands and stochastic regions. A comparison of the field structure between the SIESTA calculation and the assumption of fully penetrated vacuum perturbation indicates smaller island sizes and very small stochastic transport in the SIESTA case.