COMPARISION OF RESULTS FROM PAKAL WITH THE OBSERVATIONS FROM ALMA FOR CHROMOSPHERIC NETWORK STRUCTURES, FOCUSING ON SUB-MILLIMETER FREQUENCIES
PakalMPI is a numerical model that calculates electron and ion densities within atmospheric layers, subsequently solving the radiative transfer equation to determine solar disk brightness temperatures at various wavelengths. This code is particularly adept at simulating the solar chromosphere. Leveraging a 128-node high-performance computing cluster, we generated high-resolution solar chromosphere images at arbitrary frequencies through approximately 1000 CPU hours of computation.
This study compares synthetic emission produced by PakalMPI with contemporary observations from the Atacama Large Millimeter/submillimeter Array (ALMA). We utilized ALMA data from project ID 2018.1.01879.S , which provides temperature measurements of the chromospheric layer at a wavelength of 3 mm (approximately 100 GHz).
To enable a direct comparison, some preprocess was needed to ensure identical properties in both images from Alma and Pakal. First we needed to change units to Arcsecond and the interval of producing data which means the minimum and maximum of the temperature we are working with, the color scale, resolution and size of the image are the other properties which were changed.
By employing advanced image analysis techniques, we correlated the simulated and observed chromospheric network structures, focusing on sub-millimeter frequencies.