Fig. 3.

July 23, 2002 solar flare image reconstruction by VIS_WV with different choices for λ: panel a: λ = 0 (non-regularized solution), panel b: λ = 3.1 × 10−3 as provided by the L-curve method, panel c: λ = 5.7 × 10−3 as provided by the Miller method, and panel d: λ = 0.1 (over-regularized solution). The considered time interval is 00:29:10–00:30:19 UT, while the energy channel is 36–41 keV. Detectors from 2 through 9 have been employed.
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