A newer version of this visualization is available.
Grand Tour of the Coronal Loops Model
This is a longer coronal loops tour combining components of the two previous versions (Animation IDs 3286 and 3287). 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 which provides a snapshot of the surface at a fixed time. The resulting magnetogram is then processed through the Potential Field Source Surface (PFSS) model which constructs the magnetic field above the solar surface. The magnetic field around the Sun is then analyzed for field lines, which creates the loop structures we see in the model. Hot plasma tends to flow along the magnetic field lines, creating the coronal loops. These loops are only visible at the higher temperatures corresponding to ultraviolet light, in this case, 195 angstroms, one of the filter wavelengths of SOHO/EIT. For this version, we color the coronal loops green for ready comparison to the EIT 195 angstrom imagery using the EIT standard color table.
Please give credit for this item to:
NASA/Goddard Space Flight Center Scientific Visualization Studio
- Tom Bridgman (Global Science and Technology, Inc.) [Lead]
MissionsThis visualization is related to the following missions:
SeriesThis visualization can be found in the following series:
Datasets used in this visualization
SOHO MagnetogramID: 618Collected with Michelson Doppler Interferometer (MDI) NASA and ESA 2009-12-09
SOHO SOHO/EIT 195 (195 Filter)ID: 477Collected with Extreme-UV Imaging Telescope (EIT) NASA and ESA 2009-12-09
PFSS (Magnetic Field Lines)ID: 409Model Collected with PFSS NASA and ESA 2009-12-09
Note: While we identify the data sets used in these visualizations, we do not store any further details, nor the data sets themselves on our site.