3D-Video Products

Full disk sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 171 angstroms wavelength.	Full disk sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 195 angstroms wavelength.	Full disk sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 284 angstroms wavelength. The aftermath of the eruption of a prominence which occurred on March 24, 2007 is evident in the sequence.	Full disk sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 304 angstroms wavelength. Two promience eruptions are visible in this segment. The one on the lower right limb occurred on March 20 and the one barely visible on the disk occurred on March 24. .
Sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 171 angstroms wavelength, showing a portion of the equatorial region of the solar disk to provide a close up view of the active region.	Sequence of STEREO images from February 24, 2007 taken by the EUVI telescope in the 195 angstroms wavelength, showing a close up of an active region eruption at the limb.	Sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 284 angstroms wavelength, showing only the equatorial region of the solar disk. This provides a close up view of an large equatorial coronal hole and an active region.	Sequence of STEREO images covering March 17-March 27, 2007 taken by the EUVI telescope in the 304 angstroms wavelength, showing a portion of the equatorial region of the solar disk.
3D HD resolution animation showing 1)Results from a three dimensional computation of the magnetic field structure of an active region extrapolating the fields from measurements of the magnetic field on the surface of the Sun. This model assumes there are no electrical currents in the corona, leading to a very simple magnetic configuration. From Tahar Amari, Centre de Physique Theorique, Ecole Polytechnique, Paris. 2)Results from a three dimensional computation of the magnetic field structure of an active region extrapolating the fields from measurements of the magnetic field on the surface of the Sun. This model allows currents to flow and assumes force balance, leading to a more complex magnetic configuration for the same surface magnetic fields. From Tahar Amari. 3)Results from a three dimensional computation of the magnetic field structure of the corona extrapolating the fields from measurements of the magnetic field on the surface of the Sun. This models the corona for February 2007. Model from Pete Riley, SAIC, San Diego.