Another view of the flare over AR9906 on April 21, 2002. This version represents the full resolution of the TRACE data. This visualization represents eight hours of observing time.
Fly-in of TRACE full sun image to the flare location. Fade to a model of the field lines with a magnetogram of the solar surface. Pull back out to display a movie of flare images. This version uses lens flares to illustrate matter motion along the field lines.
Fly-in of TRACE full sun image to the flare location. Fade to a model of the field lines with a magnetogram of the solar surface. Pull back out to display a movie of flare images. This version does not show the matter motion along the field lines.
Here is a close-up view of dark tentacles or tadpoles moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE. One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare. This version of the visualization does not display the instrument clock time tags.
Here is a close-up view of dark tentacles or tadpoles moving towards the solar surface in this solar flare of April 21, 2002 seen by TRACE. One theory proposed in this press release is that they are due to voids created by magnetic reconnection in the flare. This version of the visualization displays the instrument clock time tags.
SOHO-EITs view of the Sun in late January 2005.
The solar flare at Active Region 10039 on July 23, 2002 exhibits many exceptional high-energy phenomena including the 2.223 MeV neutron capture line and the 511 keV electron-positron (antimatter) annihilation line. In the animation, the RHESSI low-energy channels (12-25 keV) are represented in red and appears predominantly in coronal loops. The high-energy flux appears as blue at the footpoints of the coronal loops. Violet is used to indicate the location and relative intensity of the 2.2MeV emission.
Close-up view of the solar active region AR9906 on April 21, 2002 with TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV.
Zoom in (with rotation) to solar active region AR9906 on April 21, 2002 with SOHO-EIT,TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV.
Zoom in to solar active region AR9906 on April 21, 2002 with SOHO-EIT, TRACE and RHESSI data. RHESSI observes x-rays from this flare. The red contours represent the 12-25 keV photon energy range and the blue contours represent 50-100 keV.
The January 20 flare began just before 2 a.m. ET. A storm of energetic protons impacted Earth just 15 minutes later. These views of the flare are from the Solar and Heliospheric Observatory (SOHO). The proton storm near Earth causes `snow in the images, obscuring the Sun as radiation swamps the cameras. The structure at the 1:30 position in the SOHO-LASCO-C3 data is the occulting disk pylon.
An image of a coronal loop from TRACE, with a co-temporal soft x-ray image from YOKOH overlaid
Zooming into the sun to show an animation of the Bastille Day solar flare from TRACE imagery
Zooming into the sun to show an animation of the Bastille Day solar flare from TRACE imagery
The TRACE spacecraft observes an X-ray flare over solar active region AR9906, April 21, 2002.
