Speaker
Description
Comprehending the horizontal velocity field of the highly magnetized plasma within the solar atmosphere is essential to understanding the complicated dynamics and energy evolution of solar phenomena at various scales, from small-scale swirls to coronal mass ejections. Most traditional methods estimate the photospheric horizontal velocity field by tracking bright features. These reconstructed velocity fields may differ from the ground truth because the photosphere is not a single layer but has a depth of $\sim$500 km. The observed bright features are combined emissions from different heights in the photosphere. In this talk, I will introduce the development of a series of models for tracking the photospheric horizontal velocity field with high accuracy from the high-resolution observations using a modified shallow U-Net architecture, and evaluate the performance of different models. All three models yield good performances, among which the hybrid model shows the best performance with a correlation coefficient of 0.85 with the ground-truth velocity field. Comparisons with the Fourier Local Correlation Tracking (FLCT) and the DeepVel methods demonstrate the superiority of the shallow U-Net models. Based on the research of this work, we have released a software named SUVEL for public use to extract photospheric horizontal velocity fields from high-resolution observations.
| Do you plan to attend in-person or online? | In-person |
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