![Figure 1: Visualization of the temperature structure across a vertical slice through a three-dimensional (3D) model of the solar atmosphere, taken from a state-of-the-art magneto-hydrodynamic simulation of the chromosphere-corona transition region (see Carlsson et al. 2016; A&A, 585, A4). The solid curve shows the heights (Z) in this model where the line-center photons of the hydrogen Lyman-α line observed by CLASP stem from (note that it practically delineates the model’s transition region). The investigation summarized in this press release demonstrates that in the true solar atmosphere the geometry of the transition region is much more complex. For more details see Trujillo Bueno and the CLASP team (2018; The Astrophysical Journal Letters, 866, L15). Figure 1: Visualization of the temperature structure across a vertical slice through a three-dimensional (3D) model of the solar atmosphere, taken from a state-of-the-art magneto-hydrodynamic simulation of the chromosphere-corona transition region (see Carlsson et al. 2016; A&A, 585, A4). The solid curve shows the heights (Z) in this model where the line-center photons of the hydrogen Lyman-α line observed by CLASP stem from (note that it practically delineates the model’s transition region). The investigat](/sites/default/files/styles/crop_square_2_2_to_320px/public/images/news/Webp.net-resizeimage%20%285%29_1.jpg?itok=lHigMxSH)
El experimento suborbital CLASP, motivado por investigaciones teóricas desarrolladas en el Instituto de Astrofísica de Canarias (IAC), ha proporcionado observaciones sin precedentes de la polarización de la radiación ultravioleta del Sol. La modelización teórica de estas observaciones pioneras ha revelado que la enigmática región de transición entre la cromosfera y la corona es extremadamente corrugada, con una geometría mucho más compleja que la de los modelos actuales de la atmósfera solar.
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