Difference between revisions of "07/14/2012 17:00:00 UTC"

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=Comment Section=
 
=Comment Section=
 +
*This is a varSITI campaign event
 
*A perfect CME-ICME chain event (J. Zhang)
 
*A perfect CME-ICME chain event (J. Zhang)
 
**classical ICME feature: shock + sheath + magnetic cloud
 
**classical ICME feature: shock + sheath + magnetic cloud
 
**strong solar signature: X1 flare (S17W08); halo CME, fast and bright
 
**strong solar signature: X1 flare (S17W08); halo CME, fast and bright
 
*Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)
 
*Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)
 +
*Time Line (2014/04/18, Jie Zhang)
 +
**07/12 15:37 UT: Flare onset;                                                0 hr
 +
**07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520);        1 hr 12 min
 +
**07/12 16:48 UT: CME first appear in C2;                            1 hr 11 min
 +
**07/12 18:54 UT: CME at 20 Rs;                                            3 hr 17 min
 +
**07/13 00:49 UT: CME at 50 Rs;                                            9 hr 12 min
 +
**07/13 06:49 UT: CME at 80 Rs;                                          15 hr 12 min   
 +
**07/14 17:00 UT: Shock arrival at 1 AU;                            49 hr 23 min
 +
**07/15 06:00 UT: Magnetic Cloud arrival at 1 AU;            62 hr 23 min
 +
**07/15 19:00 UT: Peak time of Dst (-127 nT);                    75 hr 23 min
 +
**07/17 14:00 UT: Magnetic Cloud end at 1 AU;                118 hr 23 min
 +
 +
*04/17 Discussion in Hefei-China workshop
 +
** There are possible two ejecta. The insitu data and Flux rope fitting could be found in the section of in-situ data from Wind below (2014/04/18, Yuming Wang)
 +
 +
*The event produced an intense geomagnetic storm, Dst = -127nT. [added by D. Webb]
 +
 +
*Brigitte Schmieder and her group are working on the solar aspects of this event. They are developing a data-driven simulation to explain the onset of this event and interpret the coronal signatures observed in Dudik et al., 2014. The nlfff extrapolation code is CFITS (Wheatland- Gilchrist) and the simulation is OHM (MHD code of Guillaume Aulanier et al., 2010). They will inform the group of progress. [added by D. Webb]
  
 
=Image Data=
 
=Image Data=
 +
==In-Situ Data from Wind==
 +
(Edited by Yuming Wang, 2014/04/18)
 +
 +
Two ejecta are possible.
 +
 +
[[File:overall.jpg|300px]]
 +
[[File:ejectal.jpg|300px]]
 +
[[File:ejecta2.jpg|300px]]
 +
 +
 +
** The fitted coefficients of ejecta 1 are:
 +
***  B0 = 52.098665 nT
 +
***  R = 0.28131624 AU
 +
***  Theta = -45.039456 deg
 +
***  Phi = 150.04089 deg
 +
***  H = 1.0000000
 +
***  d = -0.88881733
 +
***  t_cen = 15-Jul-2012 17:57:21 UT
 +
***  v_x = -547.26224 km/s
 +
***  v_y = -200.49954 km/s
 +
***  v_z = -36.381346 km/s
 +
***  v_exp = 226.05119 km/s, [200.91822, 225.96896]
 +
 +
** The fitted coefficients of ejecta 2 are:
 +
***  B0 = 16.776497 nT
 +
***  R = 0.056126660 AU
 +
***  Theta = -16.776502 deg
 +
***  Phi = 332.51921 deg
 +
***  H = -1.0000000
 +
***  d = -0.81328377
 +
***  t_cen = 16-Jul-2012 20:41:59 UT
 +
***  v_x = -420.51633 km/s
 +
***  v_y = -20.269702 km/s
 +
***  v_z = 26.046412 km/s
 +
***  v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]
 +
 
==In-Situ Data==
 
==In-Situ Data==
 
A combination of SWEPAM and MAG data from the ACE Satellite: <br />
 
A combination of SWEPAM and MAG data from the ACE Satellite: <br />
Line 12: Line 67:
 
[[File:plot_sw_vel_2012071400.png|350px]] <br />
 
[[File:plot_sw_vel_2012071400.png|350px]] <br />
 
The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br />
 
The blue lines are an approximation of the CME cloud and the red line denotes the shock.<br />
 +
 +
<br />
 +
The results from geometrical modeling (speeds and arrival times) in comparison to the in situ data from the Wind spacecraft (C. Moestl). The magnetic cloud is of ESW type (right handed), with the flux rope axis pointing southward; the MC has very long duration (48 hours). The shock arrival time is 2012 July 14 17:38 UT. <br />
 +
 +
[[File:Data_july122012.png|500px]]
 +
<br />
 +
 +
== Heliospheric Imaging ==
 +
CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) <br />
 +
[[File:satplot_jmap_july122012.png|400px]] <br />
 +
results of geometrical modeling (C. Moestl): <br />
 +
[[File:Geometry_12_july2012.jpeg‎|400px]] <br />
 +
 +
Jmaps along the CME leading edge position (about <math>7^{\circ}</math> S  of the ecliptic) from STEREO A and B
 +
[[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] <br>
 +
 +
De-projected Height Time Plots of the shock and ejecta fronts as obtained from the GCS (measured by Hess) (for GCS details, see Thernisien 2006) along with velocity and acceleration profiles determined from the Aerodynamic Drag Model.
 +
 +
[[File:20120712stack.png]] <br>
 +
 +
Fitting parameters in GCS Model: Carrington Longitude: 80.5738 degrees, Latitude: -8.9442 degrees, Tilt Angle: 58.1364 degrees, Aspect Ratio: .437363, Half Angular Width: 31.8636 <br>
 +
 +
[[File:20120712stereoa.gif]]
 +
[[File:20120712stereob.gif]]
  
 
==Flare Data==
 
==Flare Data==
 
*[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles
 
*[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles
 +
*Flare detection and brightness profile (double peak) by Solar Demon (joint product of AFFECTS and COMESEP FP7 projects) using SDO/AIA 94 [http://solardemon.oma.be/science/flares_details.php?delay=100&clip=1&flare_id=2989]
  
 
*GOES X-RAY FLUX
 
*GOES X-RAY FLUX
Line 21: Line 101:
  
 
=Video Data=
 
=Video Data=
 +
==SDO observations==
 +
[http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]<br>
 +
[http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] <br>
 +
[http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]<br>
 +
[http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] <br>
 +
 +
==STEREO observations==
 
[http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] <br>
 
[http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] <br>
 
[http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] <br>
 
[http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] <br>
Line 27: Line 114:
 
[http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] <br>
 
[http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] <br>
 
[http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] <br>
 
[http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] <br>
 +
 +
==PROBA2 observations==
 +
[http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] <br>
 +
[http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] <br>
 +
 +
=References=
 +
(Collected by Xin Cheng and Dave Webb)
 +
 +
1. Dudik, J. et al., ApJ, 2014,[http://adsabs.harvard.edu/abs/2014ApJ...784..144D Slipping Magnetic Reconnection during an X-class Solar Flare Observed by SDO/AIA]
 +
 +
2. Cheng, X. et al., ApJ, 2014,[http://adsabs.harvard.edu/abs/2014arXiv1405.4923C Formation of a Double-decker Magnetic Flux Rope in the Sigmoidal Solar Active Region 11520]
 +
 +
3. Moestl, C. et al., Connecting speeds, directions and arrival times of 22 coronal mass ejections from the Sun to 1 AU, ApJ, 787, 119, 2014
 +
 +
4. Hess, Phillip & Zhang, Jie, ApJ, 792, 49, 2014,[http://adsabs.harvard.edu/abs/2014ApJ...792...49H 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]
 +
 +
5. Shen, F. et al., JGR, 119, 7128, 2014
 +
 +
6. Wang, R.; Liu, Y. D.; Wiegelmann, T.; Cheng, X.; Hu, H.; Yang, Z., Relationship between Sunspot Rotation and a Major Solar Eruption on 2012 July 12, Solar Phys., DOI: 10.1007/s11207-016-0881-6, 2016.
 +
 +
7. Hu, H., Liu, Y.D., Wang, R., Möstl, C., Yang, Z.: 2016, Sun-To-Earth Characteristics of the 2012 July 12 Coronal Mass Ejection and Associated Geo-Effectiveness, Astrophys. J., 829, 97, doi:10.3847/0004-637X/829/2/97.
 +
 +
8. Marubashi, K., K.-S. Cho, H. Ishibashi: 2017, Interplanetary Magnetic Flux Rope as Agent Connecting Solar Eruptions and Geomagnetic Activities, Solar Phys., submitted.
 +
 +
9. Gopalswamy, N., Mäkelä, P., Xie, H., Yashiro, S.: 2013,Testing the empirical shock arrival model using quadrature observations, Space Weather, 11, 661–669, doi:10.1002/2013SW000945.
 +
 +
10. Webb, D., N. Nitta: 2017, Study on Understanding Problem Forecasts of ISEST Campaign Flare-CME Events, Solar Phys., submitted.

Latest revision as of 18:41, 2 March 2017

Comment Section

  • This is a varSITI campaign event
  • A perfect CME-ICME chain event (J. Zhang)
    • classical ICME feature: shock + sheath + magnetic cloud
    • strong solar signature: X1 flare (S17W08); halo CME, fast and bright
  • Propagation Direction is very close to the Sun Earth Line, making this a good event for comparing observations nearer the Sun to in-situ signatures (P. Hess)
  • Time Line (2014/04/18, Jie Zhang)
    • 07/12 15:37 UT: Flare onset; 0 hr
    • 07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min
    • 07/12 16:48 UT: CME first appear in C2; 1 hr 11 min
    • 07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min
    • 07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min
    • 07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min
    • 07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min
    • 07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min
    • 07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min
    • 07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min
  • 04/17 Discussion in Hefei-China workshop
    • There are possible two ejecta. The insitu data and Flux rope fitting could be found in the section of in-situ data from Wind below (2014/04/18, Yuming Wang)
  • The event produced an intense geomagnetic storm, Dst = -127nT. [added by D. Webb]
  • Brigitte Schmieder and her group are working on the solar aspects of this event. They are developing a data-driven simulation to explain the onset of this event and interpret the coronal signatures observed in Dudik et al., 2014. The nlfff extrapolation code is CFITS (Wheatland- Gilchrist) and the simulation is OHM (MHD code of Guillaume Aulanier et al., 2010). They will inform the group of progress. [added by D. Webb]

Image Data

In-Situ Data from Wind

(Edited by Yuming Wang, 2014/04/18)

Two ejecta are possible.

Error creating thumbnail: File missing
Error creating thumbnail: File missing
Error creating thumbnail: File missing


    • The fitted coefficients of ejecta 1 are:
      • B0 = 52.098665 nT
      • R = 0.28131624 AU
      • Theta = -45.039456 deg
      • Phi = 150.04089 deg
      • H = 1.0000000
      • d = -0.88881733
      • t_cen = 15-Jul-2012 17:57:21 UT
      • v_x = -547.26224 km/s
      • v_y = -200.49954 km/s
      • v_z = -36.381346 km/s
      • v_exp = 226.05119 km/s, [200.91822, 225.96896]
    • The fitted coefficients of ejecta 2 are:
      • B0 = 16.776497 nT
      • R = 0.056126660 AU
      • Theta = -16.776502 deg
      • Phi = 332.51921 deg
      • H = -1.0000000
      • d = -0.81328377
      • t_cen = 16-Jul-2012 20:41:59 UT
      • v_x = -420.51633 km/s
      • v_y = -20.269702 km/s
      • v_z = 26.046412 km/s
      • v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]

In-Situ Data

A combination of SWEPAM and MAG data from the ACE Satellite:

Error creating thumbnail: File missing
Error creating thumbnail: File missing
Error creating thumbnail: File missing


The blue lines are an approximation of the CME cloud and the red line denotes the shock.


The results from geometrical modeling (speeds and arrival times) in comparison to the in situ data from the Wind spacecraft (C. Moestl). The magnetic cloud is of ESW type (right handed), with the flux rope axis pointing southward; the MC has very long duration (48 hours). The shock arrival time is 2012 July 14 17:38 UT.

Error creating thumbnail: File missing


Heliospheric Imaging

CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl)

Error creating thumbnail: File missing


results of geometrical modeling (C. Moestl):

Error creating thumbnail: File missing


Jmaps along the CME leading edge position (about <math>7^{\circ}</math> S of the ecliptic) from STEREO A and B

Error creating thumbnail: File missing
Error creating thumbnail: File missing


De-projected Height Time Plots of the shock and ejecta fronts as obtained from the GCS (measured by Hess) (for GCS details, see Thernisien 2006) along with velocity and acceleration profiles determined from the Aerodynamic Drag Model.

20120712stack.png

Fitting parameters in GCS Model: Carrington Longitude: 80.5738 degrees, Latitude: -8.9442 degrees, Tilt Angle: 58.1364 degrees, Aspect Ratio: .437363, Half Angular Width: 31.8636

20120712stereoa.gif 20120712stereob.gif

Flare Data

  • File:Eve flare 2012 07 12.pdf EVE and GOES flare profiles
  • Flare detection and brightness profile (double peak) by Solar Demon (joint product of AFFECTS and COMESEP FP7 projects) using SDO/AIA 94 [1]
  • GOES X-RAY FLUX
Error creating thumbnail: File missing



The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time.

Video Data

SDO observations

AIA-94
AIA-171
AIA-211
HMI B

STEREO observations

COR2A
COR2B
HI1A
HI1B
HI2A
HI2B

PROBA2 observations

PROBA2 SWAP 174
PROBA2 SWAP 174 Difference Movie

References

(Collected by Xin Cheng and Dave Webb)

1. Dudik, J. et al., ApJ, 2014,Slipping Magnetic Reconnection during an X-class Solar Flare Observed by SDO/AIA

2. Cheng, X. et al., ApJ, 2014,Formation of a Double-decker Magnetic Flux Rope in the Sigmoidal Solar Active Region 11520

3. Moestl, C. et al., Connecting speeds, directions and arrival times of 22 coronal mass ejections from the Sun to 1 AU, ApJ, 787, 119, 2014

4. Hess, Phillip & Zhang, Jie, 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

5. Shen, F. et al., JGR, 119, 7128, 2014

6. Wang, R.; Liu, Y. D.; Wiegelmann, T.; Cheng, X.; Hu, H.; Yang, Z., Relationship between Sunspot Rotation and a Major Solar Eruption on 2012 July 12, Solar Phys., DOI: 10.1007/s11207-016-0881-6, 2016.

7. Hu, H., Liu, Y.D., Wang, R., Möstl, C., Yang, Z.: 2016, Sun-To-Earth Characteristics of the 2012 July 12 Coronal Mass Ejection and Associated Geo-Effectiveness, Astrophys. J., 829, 97, doi:10.3847/0004-637X/829/2/97.

8. Marubashi, K., K.-S. Cho, H. Ishibashi: 2017, Interplanetary Magnetic Flux Rope as Agent Connecting Solar Eruptions and Geomagnetic Activities, Solar Phys., submitted.

9. Gopalswamy, N., Mäkelä, P., Xie, H., Yashiro, S.: 2013,Testing the empirical shock arrival model using quadrature observations, Space Weather, 11, 661–669, doi:10.1002/2013SW000945.

10. Webb, D., N. Nitta: 2017, Study on Understanding Problem Forecasts of ISEST Campaign Flare-CME Events, Solar Phys., submitted.

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