Abstract
Doppler tomography is a well-known method in astrophysics to image the
accretion flow, often in the shape of thin discs, in compact binary stars. As
accretion discs rotate, all emitted line radiation is Doppler-shifted. In
fast-ion D-alpha (FIDA) spectroscopy measurements in magnetically confined
plasma, the D-alpha-photons are likewise Doppler-shifted ultimately due to
gyration of the fast ions. In either case, spectra of Doppler-shifted line
emission are sensitive to the velocity distribution of the emitters.
Astrophysical Doppler tomography has lead to images of accretion discs of
binaries revealing bright spots, spiral structures, and flow patterns. Fusion
plasma Doppler tomography has lead to an image of the fast-ion velocity
distribution function in the tokamak ASDEX Upgrade. This image matched
numerical simulations very well. Here we discuss achievements of the Doppler
tomography approach, its promise and limits, analogies and differences in
astrophysical and fusion plasma Doppler tomography, and what can be learned by
comparison of these applications.
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