Here is a video of composite SDO/AIA 171 and 131 angstrom images from 8:15 on Nov. 11, 2013 to 12:44 on Nov. 12, 2013. The small M-flare is visible in about the first sec. of the video.
The video shows the eruption with a view of the full disk with the SDO/AIA 304. Then the video zooms into a view with the SDO/AIA 193 and 304 angstrom wavelengths showing the first eruption. The video switches to a view of the second eruption in SDO/AIA 304.
This video shows the event in several SDO/AIA wavelengths. The first frames are the 304 angstrom wavelength showing the flare and a surge of southward directed darker material at temperatures around 40,000-80,000 Kelvin plasma. The next set of teal frames show the bright flash of the flare in 10-20 million Kelvin plasma with 131 angstrom light. The green images are from the 94 angstrom wavelength, showing the flare and also the southward wave in temperatures around 6 million Kelvin. The last 2 sets show 193 and 211 angstrom wavelengths. These wavelengths show 1 and 2 million Kelvin plasma respectively and are especially useful for observing coronal waves.
NASA Space Weather Research Center (SWRC) simulations indicate that the leading edge of the CME will reach Earth at about 18:39 UT on 11/12/2013 (plus minus 7 hours). The geomagnetic impact is expected to be minor at most.
The event was similar to the earlier X3.3. It was impulsive and compact but not as much as the X3.3 flare. This eruption produced a small but noticeable coronal wave and dimming, indicating the loss of material in the form of a coronal mass ejection (CME.) The eruption also produced Type II and IV radio bursts, typical of a CMEs associated with a flare and a CME/radiation storms respectively. There was a moderately bright CME observed in the SOHO/LASCO and STEREO A&B Cor2 instruments. The CME was southward directed instead of Earth-directed despite the region's location on the solar disk.
The video shows the eruption with a view of the full disk with the SDO/AIA 304,171 and 193 angstrom wavelength then a zoomed in view with the SDO/AIA 171, 193 and 131 angstrom wavelengths.
This video starts with a close-up of the region over about 24 hours. This part of the video is created from composites of 171, 193 and 131 angstrom images. The second part is just 171 angstrom and is only over 4 hours around the event. These videos show the compact, impulsive nature of the flare. Also, if you look closely at the highlighted magnetic loops in the 171 images you can see that after the flare, they don't move around or wiggle very much. So basically you are not seeing a lot of material moving around. For a large, strong CME you would expect to see a lot of "stuff" moving around as well as waves that would move the magnetic field lines around.
- NASA Goddard Space Flight CenterHeliophysicist, 2005 - present
- L-3 Communications (NASA GSFC)Solar Astrophysicist, 2003 - 2005
- Emergent Information Technologies (NASA/GSFC)Solar Astrophysicist, 2000 - 2003
- Florida State UniversityBachelor of Science in Physics, 1987 - 1991
- University of New HampshireMasters of Physics, 1992 - 1995
- University of New HampshireDoctor of Philosophy in Physics, 1995 - 2000
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