2015/06/28 by Gregory D. Fleishman, Fleishman, Gregory, M. Loukitcheva +3
Physics and Astronomy · #FOS: Physical sciences #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.1506.08395
openalex publication_date 2015/06/28 · openalex created_date 2020/07/23 · openalex updated_date 2026/07/28
We developed an efficient algorithm integrated in our 3D modeling tool, GX\nSimulator (Nita et al. 2015), allowing quick computation of the synthetic\nintensity and polarization maps of solar active regions (AR) in the ALMA\nspectral range. The algorithm analyzes the photospheric input (white light and\nmagnetogram) to classify a given photospheric pixel to belong to a given\nphotospheric structure. Then, a 1D chromospheric model (Fontenla et al. 2009)\nis added on top of each pixel, which forms a chromospheric model of the AR.\nNext step is computation of the mm and sub-mm emission produced from this\nchromosphere model. A huge advantage of this approach is that emission from any\ngiven AR can be synthesized very fast, on the order of a few minutes after the\nAR selection. Using the GX Simulator tool it is also possible to produce\nsynthetic maps of the microwave (gyroresonance) and EUV emission from the same\nAR model and compare them with the ALMA synthetic maps and with the\ncorresponding observed microwave and/or EUV data.\n