Synopsis
A slow rotating tour of a data-based coronal loop model. The solar model is constructed from magnetogram data collected by SOHO/MDI. Because we do not see the full solar surface at any one time, the magnetograms collected over the course of a solar rotation are processed through a time-evolving solar surface model to provide a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model. Coronal loops are visible at the higher temperatures of ultraviolet light, in this case, 195 ‘Ê_ngstroms, the filter wavelength of SOHO/EIT. The frames were generated for an experimental color stereo projection system. . Data Collected: December, 2001. Animator: Tom Bridgman (GST). Scientist: Russ Howard (NRL), Michael Kaiser (NASA/GSFC), Therese Kucera (NASA/GSFC), Don Michels (NRL). Platforms/Sensors/Data Sets: PFSS/Magnetic Field Lines, SOHO/Extreme-UV Imaging Telescope (EIT)/195 Angstroms, SOHO/Michelson Doppler Interferometer (MDI)/Magnetogram.
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