Luc Rouppe van der Voort

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Sunspot umbrae--the dark central regions of the spots--are surrounded by brighter filamentary penumbrae, the existence of which remains largely inexplicable. The penumbral filaments contain magnetic fields with varying inclinations and are associated with flowing gas, but discriminating between theoretical models has been difficult because the structure of(More)
The solar chromosphere and transition region (TR) form an interface between the Sun's surface and its hot outer atmosphere. There, most of the nonthermal energy that powers the solar atmosphere is transformed into heat, although the detailed mechanism remains elusive. High-resolution (0.33-arc second) observations with NASA's Interface Region Imaging(More)
Heating the outer layers of the magnetically quiet solar atmosphere to more than one million kelvin and accelerating the solar wind requires an energy flux of approximately 100 to 300 watts per square metre, but how this energy is transferred and dissipated there is a puzzle and several alternative solutions have been proposed. Braiding and twisting of(More)
We present examples of the application of the image restoration method of Multi-Object Multi-Frame Blind Deconvolution to observations obtained with the Swedish 1-m Solar Telescope on La Palma. This restoration method is an extension of Joint Phase Diverse Speckle image restoration. Multiple realizations of multiple objects can now be restored jointly,(More)
With the recent advent of the Swedish 1-m Solar Telescope (SST), advanced image processing techniques, as well as numerical simulations that provide a more realistic view of the chromosphere, a comprehensive understanding of chromospheric jets such as spicules, mottles and fibrils is now within reach. In this paper, we briefly summarize results from a(More)
We have obtained high-resolution spectrograms of small-scale magnetic structures with the Swedish 1-m Solar Telescope. We present Doppler measurements at 0.2 00 spatial resolution of bright points, ribbons, and flowers, and their immediate surroundings, in the C i k5380.3 line (formed in the deep photosphere) and the two Fe i lines at 5379.6 and 5386.3 8.(More)
Context. For many years, there seemed to be significant differences between the continuum intensity distributions derived from observations and simulations of the solar photosphere. Aims. In order to settle the discussion on these apparent discrepancies, we present a detailed comparison between simulations and seeing-free observations that takes into(More)
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