Difference between revisions of "03/17/2013 05:30:00 UTC"
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| − | [http://solar.gmu.edu/wiki/upload/phess4/20120315aia171.mp4 AIA 171] | + | [http://solar.gmu.edu/wiki/upload/phess4/20120315aia171.mp4 AIA 171] <br> |
| − | [http://solar.gmu.edu/wiki/upload/phess4/20120315aia193.mp4 AIA 193] | + | [http://solar.gmu.edu/wiki/upload/phess4/20120315aia193.mp4 AIA 193] <br> |
| − | [http://solar.gmu.edu/wiki/upload/phess4/20120315hmi.mp4 HMI] | + | [http://solar.gmu.edu/wiki/upload/phess4/20120315hmi.mp4 HMI] <br> |
=References= | =References= | ||
Revision as of 13:57, 19 June 2014
Contents
Comment Section
- This is a varSITI campaign event
- Depressed density and temperature as well as decreasing velocity are indicative of a flux rope, but with the weak magnetic field it may just be the flank passing through the Earth. Clear shock signatures in temperature and velocity and total B, more of a gradual increase in density. (Hess)
Image Data
In-Situ Data
A combination of SWEPAM and MAG data from the ACE Satellite:
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The blue lines are an approximation of the CME cloud and the red line denotes the shock.
Heliospheric Imager Data
