2D DC potential structures induced by RF sheaths coupled with transverse currents in front of ICRF antennas

12th International Congress on Plasma Physics, 25-29 October 2004, Nice (France)Sheaths are space charge regions at the plasma-wall. They are induced by the differential inertia between ions and electrons, and without external perturbation, they create a floating potential between the neutral plasma and the walls. In Tokamaks, these sheaths are locally enhanced by the RF (radiofrequency) electric field generated by the ICRF (ion cyclotron resonance frequency) antennas used to heat magnetic fusion plasmas at very high temperature. RF sheaths are located at the connection points of magnetic field lines to the wall, or to the bumpers which protect the antenna or to any part of the antenna structure. The asymmetric behaviour of these oscillating sheaths rectifies RF potentials in the plasma in front of antenna, to finally create nonlinearly a DC potential which can be much higher than the floating potential. We study specifically how the space-time distribution of these RF and DC rectified potentials is modified when nearby flux tubes are allowed to exchange perpendicular polarization current. To simulate that, a 2D fluid code has been implemented to compute the 2D RF potential map in a plane perpendicular to magnetic lines, and within the flute approximation the whole 3D potential map is deduced. In simulation, we consider a homogeneous transverse conductivity and use a “test” potential map having, in absence of transverse currents, a Gaussian shape characterized by its width r0 and its amplitude f0. As a function of these 2 parameters (normalized respectively to a characteristic length for transverse transport and to the local temperature), we can estimate the peaking and the smoothing of the potential structure in the presence of polarization current. So, we are able to determine, for typical plasmas, the amplitude of DC potential peaks , particularly on antenna's corners , where hot spots appear during a shot. In typical Tore Supra conditions near antenna corners potential structures less than centimetric are involved in the 2D effects. The next step will consist in studying space transition between several areas characterized by different perpendicular conductivities, which can be modelled via effective connection lengths in our 2D fluid code. This more precise approach will be useful to obtain the potential structures in front of each part of the complex antenna's geometry and to minimize potential peaks generating many spurious perturbations in the plasma edge for long duration discharge as in ITER reactor

Impact of minority concentration on fundamental (H)D ICRF heating performance in JET-ILW

ITER will start its operation with non-activated hydrogen and helium plasmas at a reduced magnetic field of B-0 = 2.65 T. In hydrogen plasmas, the two ion cyclotron resonance frequency (ICRF) heating schemes available for central plasma heating (fundamental H majority and 2nd harmonic He-3 minority ICRF heating) are likely to suffer from relatively low RF wave absorption, as suggested by numerical modelling and confirmed by previous JET experiments conducted in conditions similar to those expected in ITER's initial phase. With He-4 plasmas, the commonly adopted fundamental H minority heating scheme will be used and its performance is expected to be much better. However, one important question that remains to be answered is whether increased levels of hydrogen (due to e. g. H pellet injection) jeopardize the high performance usually observed with this heating scheme, in particular in a full-metal environment. Recent JET experiments performed with the ITER-likewall shed some light onto this question and the main results concerning ICRF heating performance in L-mode discharges are summarized here

Modelling of the ICRF induced E x B convection in the scrape-off-layer of ASDEX Upgrade

In magnetic controlled fusion devices, plasma heating with radio-frequency (RF) waves in the ion cyclotron (IC) range of frequency relies on the electric field of the fast wave to heat the plasma. However, the slow wave can be generated parasitically. The electric field of the slow wave can induce large biased plasma potential (DC potential) through sheath rectification. The rapid variation of the rectified potential across the equilibrium magnetic field can cause significant convective transport (E x B drifts) in the scrape-off layer (SOL). In order to understand this phenomenon and reproduce the experiments, 3D realistic simulations are carried out with the 3D edge plasma fluid and kinetic neutral code EMC3-Eirene in ASDEX Upgrade. For this, we have added the prescribed drift terms to the EMC3 equations and verified the 3D code results against the analytical ones in cylindrical geometry. The edge plasma potential derived from the experiments is used to calculate the drift velocities, which are then treated as input fields in the code to obtain the final density distributions. Our simulation results are in good agreement with the experiments

GRB 110205A: Anatomy of a long gamma-ray burst

The Swift burst GRB 110205A was a very bright burst visible in the Northern hemisphere. GRB 110205A was intrinsically long and very energetic and it occurred in a low-density interstellar medium environment, leading to delayed afterglow emission and a clear temporal separation of the main emitting components: prompt emission, reverse shock, and forward shock. Our observations show several remarkable features of GRB 110205A : the detection of prompt optical emission strongly correlated with the BAT light curve, with no temporal lag between the two ; the absence of correlation of the X-ray emission compared to the optical and high energy gamma-ray ones during the prompt phase ; and a large optical re-brightening after the end of the prompt phase, that we interpret as a signature of the reverse shock. Beyond the pedagogical value offered by the excellent multi-wavelength coverage of a GRB with temporally separated radiating components, we discuss several questions raised by our observations: the nature of the prompt optical emission and the spectral evolution of the prompt emission at high-energies (from 0.5 keV to 150 keV) ; the origin of an X-ray flare at the beginning of the forward shock; and the modeling of the afterglow, including the reverse shock, in the framework of the classical fireball model.Comment: 21 pages, 5 figure (all in colors), accepted for publication in Ap