The training data used to create such technology were three different numerical simulations of turbulent convection. This means that we could feed it solar data and expect that the results it returns are consistent with what is actually occurring on our fascinating, forbidding star. They found that based solely on the temperature and vertical flow data, the AI could accurately describe horizontal flows in the simulations that would be undetectable on the real Sun. The method consists of multiple convolutional kernels with various sizes of receptive fields and performs convolution for spatial and temporal axes. To predict the horizontal velocities for each convection simulation researchers created a multi-scale deep learning architecture. This is due to the hot plasma that rises in the middle of the Sun and then falls back around the edges where it cools off. This layer is very multifaceted in the sense that some of the parts of the photosphere are very dark on one end and light on the other side and many shades in between. This is where all of the sunspots, solar flares, and other activities take place. What we, in layman’s terms, call the surface of the Sun is actually called the photosphere. This could help us to better understand solar convection, and processes that generate explosions and jets erupting from the Sun. Basically, Fed only temperature and vertical motion data collected from the surface of the solar photosphere, the AI model could correctly identify turbulent horizontal motion below the surface. However, this velocity component can be calculated with the help of AI and that’s the biggest breakthrough that was obtained in this new research.
While it is possible to get some measurements of the velocity through the Doppler shifts, it is difficult to obtain the velocity component perpendicular to the line of sight, which corresponds to the horizontal velocity in disk center observations. It is important to derive three-dimensional velocity vectors to understand the nature of the turbulent convection and to evaluate the vertical Poynting flux toward the upper atmosphere. The dynamics in the photosphere are governed by the multi-scale turbulent convection termed granulation and supergranulation. Estimating Horizontal Velocity Fields on the Solar Surface
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