Difference between revisions of "03/31/2015 07:31:49 UTC"
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=Comment Section= | =Comment Section= | ||
*Clear shock, followed by most of the standard MC signatures (low beta, low density, smooth magnetic field, etc.), but a fairly weak magnetic field rotation. <br> | *Clear shock, followed by most of the standard MC signatures (low beta, low density, smooth magnetic field, etc.), but a fairly weak magnetic field rotation. <br> | ||
| − | *At 03/27/2015 15:12:08, there may be a partial halo CME corresponding to this magnetic cloud. The solar source of this CME is unknown. | + | *At 03/27/2015 15:12:08, there may be a partial halo CME corresponding to this magnetic cloud. The solar source of this CME is unknown. (Yutian) |
| − | (Yutian) | ||
=Image Data= | =Image Data= | ||
A combination of MFI and SWE data from the Wind Satellite: <br /> | A combination of MFI and SWE data from the Wind Satellite: <br /> | ||
| + | |||
| + | [[File:Example.jpg|400px]] | ||
The grey region shows an approximation of the CME cloud and the red vertical line denotes the shock. | The grey region shows an approximation of the CME cloud and the red vertical line denotes the shock. | ||
Latest revision as of 11:14, 18 September 2017
Comment Section
- Clear shock, followed by most of the standard MC signatures (low beta, low density, smooth magnetic field, etc.), but a fairly weak magnetic field rotation.
- At 03/27/2015 15:12:08, there may be a partial halo CME corresponding to this magnetic cloud. The solar source of this CME is unknown. (Yutian)
Image Data
A combination of MFI and SWE data from the Wind Satellite:
Error creating thumbnail: File missing
The grey region shows an approximation of the CME cloud and the red vertical line denotes the shock.
