ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Observatory O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: of the proxy of the chromospheric heating and maxima of green lines show the regions with the maximum of the proxy of the photospheric heating. The arrows connecting these maxima show their spatial displacement. In three cases out of four, the arrow orientation is in agreement with our estimation of the spatial displacement of the photospheric and chromospheric heating. The spatial separation of the maxima is between 0ʺ̣5 and 1′′. We note that the local maxima of the black lines for the orange and green streamlines located around 3′′ and 2ʺ̣5, respectively, are caused by the evolution of the light bridge intensity and are not related to the WLF. Only in one case (cyan streamline) does the arrow point in a direction that is not in agreement with our interpretation of the projection effect. It should be noted that although the results presented in Fig. 12 are mostly in agreement with our expectations, they cannot be taken as confirmation of the projection effect. The used proxies do not represent the chromospheric and photospheric heating accurately. The magnetic field configuration is more complex and not retrieved precisely with our height-independent model atmosphere. The energy deposition along the field lines is dependent on the physical properties of the chromosphere that are unknown and can differ from pixel to pixel. In addition, the location of the flare-loop footpoints where beams of accelerated particles propagated is not known because imaging hard X-ray data are not available during the time of the Hinode flare scan. Thus, the nature of the atmospheric heating cannot be identified either. 5. Conclusions We use a unique dataset obtained by the Hinode satellite capturing the X9.3-class WLF ribbon with a spectropolarimetric raster scan. The observed Stokes profiles allow us to interpret the temperature stratification of the solar photosphere during this WLF under the assumption of LTE conditions. Comparing these data with temperatures obtained in the post-WLF phase, we can also estimate the heating of the photosphere during the WLF. In the studied WLF ribbon, the flare affected also the upper photosphere. In pixels with the most enhanced emissions, the photosphere is heated down to log τ = −0.5, i.e. approximately 80 km above the solar surface. This is in agreement with the shape of the Stokes I profiles in these pixels as the Fe I lines show absorption features in the far wings, i.e. it signifies a temperature decrease around log τ = 0. Nevertheless, we observe enhancements of the continuum intensity equivalent to that can be ascribed to the WLF ribbon. This corresponds in certain pixels to an increase of I c by 200% (see Figs. 3 and 9 ). Following the analogy of the study by Heinzel et al. (2017) , we assume that this continuum contribution is mostly due to the Paschen recombination continuum formed in the chromosphere. However, we are aware that there are studies locating the WLF sources at various layers in the photosphere (