03/17/2015 04:00:00 UTC
Contents
Comment Section
- varSITI campaign event
- Largest geomagnetic storm at Earth for solar cycle 24, this event registered a Dst peak of -228 nT.
- Based on both the in-situ signature of the event and the ENLIL solar wind prediction for this date, I think it is likely a CIR played a role in making it so strong. There is a strong coronal hole at the South Pole and the ENLIL simulation ([[1]]) shows a fairly fast stream that interacts with the CME, and this fast speed stream (~600 km/s) shows up in ACE data as well. Based on the C2 and C3 images for the day, it appears there is a slow CME launching around noon on the 14th with a small but visible filament. On the morning of the 15th a partial halo CME, associated with a long duration flare that fell just short of M class (C9.1) and from the same active region (AR 12297), launched propagating to the East of the Sun Earth line. I think it is likely that an interaction between the CME+shock of this event and the previous blob CME, as well as the added energy from the CIR and fast speed stream behind the CME caused the severity of the geomagnetic activity at the Earth (Hess)
- This super storm is produced through a combination of effects: (1) strong magnetic field in the sheath region (> 25 nT at peak)) and ejecta (>30 nT at peak, (2) Bs field encompasses the entire duration of the ejecta, due to that the axis of the flux rope is highly inclined toward the north-south direction, (3) the interaction with CIR, and almost contained in a CIR region. Such containment by CIR prevents the expansion of the flux rope, thus makes the flux rope small in size by strong in magnetic field (Jie Zhang).
- This may be a kind of CME-CME interaction event. We have a large filament, embedded in a magnetic flux rope, close to the AR which released this highly geoeffective CME. Part of the filament (or flux rope) erupted - or at least, left the low corona - already on March 14 (around 12UT). The final and major eruption on March 15 seems to interact with the first disturbance. The interacting sectors might propagate close to Earth direction. This might be a reason for the complex in-situ signatures (two flux ropes?) as well as the increased geoeffectiveness (Manuela Temmer).
Image Data
In-situ data
- These are in-situ plots based on the ACE daily text files, I will update them when the cdf data becomes available. In these plots the shock is very clear, but beyond that any ejecta signature is weak and there does not appear to be any strong Magnetic cloud. But there are two clear and distinct periods of strong -Bz. (Hess)
LASCO/Kanzelhöhe
GOES Plot
Video Data
AIA 171 movie
AIA 193 movie
AIA 304 movie
AIA 1600 movie
HMI movie
C2 movie
C3 movie
