Working Group 4
Campaign Event Group led by Dave Webb (USA), Nariaki Nitta (USA) and Luciano Rodriguez (Belgium).
A brief summary of the activity of WG4 at the workshop can be found here.
- 1 Objectives
- 2 Scientific Questions, Technique Approach/Methodology
- 2.1 What are the common issues when linking ICMEs to CMEs?
- 2.2 Calculating arrival times
- 2.3 When/why will a full halo CME not arrive to the Earth?
- 2.4 When/why will a narrow CME (as seen from L1) arrive to the Earth?
- 2.5 What solar parameters can we use to provide an estimation of geoeffectivity?
- 2.6 More interesting topics:
- 2.7 Working list and details of events
- 3 Updated WG4 Events as of May 2016 [D. Webb]
- 4 As of September 2015 [D. Webb]
- 5 Selected campaign events
- 6 Future Plan
- Provide textbook-style standard CME-ICME chain events from the Sun to the Earth based on the state-of-the-art observations and successful theoretical analysis and numerical simulation: happy stories
- Examine controversial Earth-Affecting CME/ICME pairs during the STEREO era (from 2007): surprising stories
- To analyse the complications that arise when linking CMEs to ICMEs
- To obtain new insights that could be applied when forecasting ICME arrivals at the Earth
- Integrate theory, simulations and observations in order to get a complete view of the chain of events from the Sun to the Earth
Scientific Questions, Technique Approach/Methodology
- Multiple events
- Stealth CMEs
- CME deflection
Calculating arrival times
- Projected vs 3D speeds
- Propagation models (DBM, ENLIL, etc.)
- Error margins
When/why will a full halo CME not arrive to the Earth?
When/why will a narrow CME (as seen from L1) arrive to the Earth?
What solar parameters can we use to provide an estimation of geoeffectivity?
More interesting topics:
- Forbush decreases (Mateja, Dragan, Darije)
- Sympathetic flares (Nariaki)
- SEPs (Bernd?)
- Prominence material in ICMEs, signatures in compositional data (Luciano)
- Determination of S/C path through the ICME, central or flank crossings
- Use of remote data to infer Bz: magnetograms, extrapolations, flux rope orientation
- False alarms: CMEs that did not arrive to the Earth when they were expected to, and viceversa.
Working list and details of events
Updated WG4 Events as of May 2016 [D. Webb]
As of September 2015 [D. Webb]
• VarSITI-wide campaign study events:
1. 2012 July 12-14 CME. This event is selected by ISEST.
This is a textbook (TB) style event, with a clear chain of activity signatures all the way from the solar surface, inner corona and outer corona (X1.4 flare and fast CME), to in-situ near the Earth (a shock and magnetic cloud [MC]). Also of interest are the 2012 July 23-24 and other events from the same active region.
It produced an intense geomagnetic storm, Dst = -127nT. In a prior ISEST workshop, we agreed to study this event extensively.
References: Dudik, J. et al., ApJ, 2014; Cheng, X. et al., ApJ, 2014; Moestl, C. et al., ApJ, 787, 119, 2014; Hess, P. & Zhang, J., ApJ, 792, 49, 2014 Stereoscopic Study of the Kinematic Evolution of a Coronal Mass Ejection and Its Driven Shock from the Sun to the Earth and the Prediction of Their Arrival Times; Shen, F. et al., JGR, 119, 7128, 2014;
2. 2012 October 4-8 CME. This event has been recommended by ISEST and SPeCIMEN.
This is an excellent stealth CME, i.e., a strong CME in the inner corona and ICME, but the solar disk signatures are multiple and weak, and it had slow propagation to Earth. At Earth a smaller storm, Dst=-105. Electron acceleration in the radiation belt has been studied by Reeves, G.D. et al (2013). (P)roblem event.
URL: http://solar.gmu.edu/heliophysics/index.php/10/08/2012_05:00:00_UTC References:
3. 2013 March 15-17 CME. Recommended by ISEST and SPeCIMEN.
At the Sun an M1.1 flare, erupting filament, type IV radio burst, fast halo CME. At Earth a shock, possible MC, SEP, and strong storm, Dst=-132. TB case. Modeled by C-C Wu.
4. 2013 June 1 CME. Recommended by ISEST and ROSMIC.
Possibly due to a slow CME on May 27 Coronal hole influence? Cause of big storm unclear, Dst=-119. P.
5. 2015 March 15-17 CME. This event is selected by ISEST.
First “super” storm of SC24 was caused by an Earth-directed CME that erupted on 15 March 2015 from near disk center (S18W39) with a speed of 1120 km/s in the sky plane. N. Gopalswamy – this can be converted to an earthward speed of ~1025 km/s based on the source location on the Sun. The CME arrived with a MC on March 17 at 13:38 UT with a large southward field in the sheath (-15 nT) and in the front of the cloud (-25 nT). There were Dst dips corresponding to the sheath and cloud portions, with the deepest minimum Dst of 223 nT occurring at 23:00 UT on March 17. The speed of the MC was ~600 km/s, considerably smaller than the white-light CME speed of 1025 km/s.
Refs: Gopalswamy et al., Proc. 14th International Ionospheric Effects Symposium, May 12-14, 2015, Alexandria, VA.; Wu et al., abs. for the SCOSTEP-WDS Workshop at NICT, Japan, Sept, 2015; Jackson, priv. comm.; Kamide, Y & K. Kusano, Space Weather, 13, 2015; Liu, Y. at al., Plasma and Magnetic Field Characteristics of Solar Coronal Mass Ejections in Relation to Geomagnetic Storm Intensity and Variability, subm. ApJL, arXiv:1508.01267v1; Kataoka, R., D. Shiota, E. Kilpua, K. Keika, JGR-A, accepted, July 2015; P. Gallagher press release: http://files.mail-list.com/m/iswinewsletter/2015-07-space-weather-scans-solar-storms.pdf.
6. 2015 June 22-24 CME. This event is selected by ISEST.
Second “super” storm of SC24, and this year, was caused by an Earth-directed CME that erupted on 22 June 2015 from near disk center () with a speed of km/s in the sky plane. Compound event with a series of shocks arriving over a 3-day span, and one likely magnetic cloud arriving around midnight on the 23rd, corresponding to a clear, symmetric halo CME on the 21st which drove the strongest of the shocks with a highly compressed magnetic field. Drove a powerful geomagnetic storm with a Dst =195.
N. Lugaz: The first dip on June 22nd (~-150 nT) is clearly due to a shock propagating in preceding CME... The larger dip on the 23rd is due to the following CME... There are three probable fast forward shocks in 30 hours from 06/21 at 15UT to 06/22 at 18UT. The third shock combines a very large increase in dynamic pressure and a large short-duration southward Bz; it must have really compressed the magnetosphere like crazy. The CME on the 23rd had extremely low density and back of the envelope estimate shows that the solar wind may have had a Mach number of ~1.
N. Nitta: There were at least four eruptions during 18-22 June and the third one (associated with a M2 flare on 21 June) was a quite impressively circular CME, which I think contributed the most to the geo-space effects (the CME arrived much earlier than I had thought). Three CMEs seemed to have arrived without merging,.. The M6.5 flare on 22 June was not associated with a very geo-effective CME even though it arrived fast.
Y. Liu: This is actually a multi-step geomagnetic storm… The first dip was produced by the fluctuating southward field components upstream of the third shock, the second one by the southward field components downstream of the third shock, and the major one by the southward field components within the ICME associated with the June 21 M2.0 eruption (01:42 UT). I agree with Nariaki that the June 22 M6.5 eruption didn't produce obvious geo-effectiveness... The fourth shock in the plot was associated with the June 22 M6.5 eruption, and it was beginning to overtake the ICME from behind at 1 AU. Another eruption on June 25 (M7.9) also produced a shock that impacted Earth.., but wasn’t geo-effective either.
E. Kilpua: The strongest Bs intervals and the Dst minimum in the June event are … preceded by a mainly northward IMF and high density in CME sheath. Such conditions combined may have led to particularly dense plasma sheath and enhanced the ring current later when strong Bs related to FR1 (in Ying's plot) arrived.
Refs.: Liu, Y. at al., Plasma and Magnetic Field Characteristics of Solar Coronal Mass Ejections in Relation to Geomagnetic Storm Intensity and Variability, subm. ApJL, arXiv:1508.01267v1.
• Other ISEST WG4 events being studied:
7. 2012 March 7-9.
An X5 flare, wave, fast CME. At Earth a shock, magnetic cloud (MC), and strong storm, Dst=-131. TB case. Of interest because of the influence of a CH on a relatively modest CME.
8. 2012 July 23-24
This was the famous energetic, very fast event directed at STEREO-A. There were two consecutive prominence eruption/flares starting about 02:20 UT on July 23, seen best in SOHO and STEREO-B observations. The shock hit STEREO-A on July 23, 20:55 UT, followed by two ICMEs, the first starting about 23:00 UT and the second at 01:51 UT on July 24.
- N. Nitta says “It was not an Earth-affecting event, but it was said to have possibly been as geoeffective as the Carrington event had it occurred 9 days earlier [and been aimed at Earth-DW]. I think it is important to understand the interplanetary conditions as disturbed by AR 11520 over an extended period.”
- M. Temmer: “i am currently working together with Nariaki on the complex (two-step) eruption from July 23, 2012 event aiming to simulate the short arrival time and high impact speed by using the analytical drag-based-model. the low density in interplanetary space as well as the high mass of the CME might be the decisive factors for this event to be so fast. The question remains whether the event from July 19 is able to lower the density over several days and as such is able to change the interplanetary conditions. i had during the process of the analysis nice discussions with Ying Liu and Janet Luhmann. We would like to encourage people to take a closer look on this event. We had subjective interpretations of the white-light structures, but most important found no conclusion on the high magnetic field as measured in-situ for both magnetic structures. Is it maybe something intrinsic to the active region? … it would be good to get modelers involved for gaining some deeper insight into the complex eruption process and its in-situ effects.”
URL: http://solar.gmu.edu/heliophysics/index.php/07/23/2012_23:00:00_UTC Refs: Russell, C. et al., ApJ, 770, 38, 2013; Ngwira, C. et al., GRL, 2013; Baker, D., Space Weather, 11, 585, 2013; Liu, D.L. et al., NComm., 5, 4381, 2014; Gopalswamy et al., E,P&S, 66, 104, 2014; Temmer and Nitta, Solar Phys., 290, 919, 2015;
9. 2014 January 6, 07:30, WL: Produced a GLE (see next).
- N. Gopalswamy reports that the January 6 and 7 CMEs are quite intriguing. The Jan. 6 event produced a GLE even though it had a speed <2000 km/s and originated behind the west limb (Thakur et al. 2014).
URL: Refs: Thakur et al., ApJL, 2014
10. 2014 January 7-9
A “problem” event being studied for a Fall 2014 AGU session: SH51E: Challenges to Space Weather Forecasting and Data-Driven Modeling of the Sun Focused on January 2014; 19 Dec. 2014 (e.g., Webb, 2014).
The Jan. 7 CME was assoc. with a X1.2 flare near disk center (S12W08) and was ultrafast (~2400 km/s), but was likely deflected to the south and west so it was not geoefffective. It was a large SEP event, but not a GLE. The shock and sheath were likely detected at Earth (9, 19:40 UT) and Mars (10, 22:30 UT) – Moestl et al. (2015).
Ref: Webb, An Overview of the 7 January 2014 X-Class Flare-CME and Space Weather Predictions, AGU SH51E-01, 2014; Moestl et al., Nat. Commun., 6, 7135, 2015; Gopalswamy et al., E,P&S, 66, 104, 2014;
11. 2014 September 10-13
An X1.6 flare and wave near Sun Center and a nearly symmetric halo CME. The evolution of the source active region (AR 12158) is also of interest.
The ICME at L1 on 12-13 Sept. mostly had strong northward field in the putative flux rope (several models produced). The southward fields, which drove the early storm activity, were in the sheaths trailing two IP shocks, the second one being the strongest. The ICME north field rapidly shut down the auroral and storm activity.
A STEREO SWx Group event. “U” case? B. Jackson runs a real time forecast site, and have included the Rosetta comet mission in the forecasts, currently using IPS data. A density response at Rosetta due to the Sept. 10 event was predicted for IPS and modeled using the ENLIL 3D-MHD code. We are looking for Rosetta solar wind data to confirm an ICME there.
Refs.: McKenna-Lawlor et al. EM&P, subm, 2015; B. Jackson, priv. comm.;
- WG1 events
Selected campaign events
- Textbook example: 12 July 2012
- Problematic event: 5 October 2012 (stealth CME, ICME trailed by a HSS)
- Backup problematic event: June 7 2013 (MC a bit weak)
- Collect results of simulations and models
- Compare and integrate simulations results with observations
- Start/continue the work related to the scientific questions