heliophysics - User contributions [en]

07/14/2012 17:00:00 UTC

2013-08-30T10:46:42Z

Adevos:

=Comment Section=
*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)

=Image Data=
==In-Situ Data==
A combination of SWEPAM and MAG data from the ACE Satellite: 
[[File:plot_sw_mag_plasma_2012071400.png|350px]]
[[File:plot_sw_mag_2012071400.png|400px]]
[[File:plot_sw_vel_2012071400.png|350px]] 
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. 

[[File:Data_july122012.png|500px]]
 

== Heliospheric Imaging ==
CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) 
[[File:satplot_jmap_july122012.png|400px]] 
results of geometrical modeling (C. Moestl): 
[[File:Geometry_12_july2012.jpeg‎|400px]] 

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]] 

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]] 

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 

==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 [http://solardemon.oma.be/science/flares_details.php?delay=100&clip=1&flare_id=2989]

*GOES X-RAY FLUX
[[File:20120712_goes.png|500px]] 
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==
[http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94] 
[http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] 
[http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211] 
[http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] 

==STEREO observations==
[http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] 
[http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] 
[http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] 
phess4/hi1Brd.avi HI1B] 
[http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] 
[http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] 

==PROBA2 observations==
[http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] 
[http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] 

=References=

10/08/2012 05:00:00 UTC

2013-08-30T10:34:16Z

Adevos:

=Comment Section=
*A good ICME, strong CME source, however, "stealth" surface signature (J. Zhang)
**A good example of "stealth" CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)
*This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)
* M. Temmer: clear on-disk signatures - movie from SDO - are visible. It is a "silent" CME, hard to catch for space weather forecasters, but not a "stealth" in sense of no solar surface signatures at all.
http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov [October 4, 15UT, central south]
*C. Moestl: looking at the whole October 4 SDO movie, there are also two other minor eruptions which I find very hard to distinguish from the 15 UT one (1. 7 UT, slightly west of disk center; 2. 0930 UT, south-east quadrant)
* timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail
* these eruptions are also visible in the SWAP data (http://proba2.oma.be/), including another minor one at 14h UT in the south-east quadrant (A. Devos)

=Image Data=
==In-Situ Data==
A combination of SWEPAM and MAG data from the ACE Satellite: 
[[File:plot_sw_mag_plasma_2012100700.png|350px]]
[[File:plot_sw_mag_2012100700.png|400px]]
[[File:plot_sw_vel_2012100700.png|350px]] 
The blue lines are an approximation of the CME cloud and the red line denotes the shock.

==Jmaps==
Jmaps from STEREO A and B along the CME leading edge position angle 

[[File:jmapA20101005.jpg|500px]]
[[File:jmapB20101005.jpg|500px]]

 

=Video Data=
[http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] 
[http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] 
[http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] 
[http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] 
[http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] 
[http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] 
[http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] 
[http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] 
[http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] 
[http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_movie.mp4 PROBA2 SWAP 174] 
[http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] 

=References=

10/08/2012 05:00:00 UTC

2013-08-30T10:33:36Z

Adevos:

=Comment Section=
*A good ICME, strong CME source, however, "stealth" surface signature (J. Zhang)
**A good example of "stealth" CME: bright CME, but no or very weak surface signature (in terms of no flare, dimming, filament eruption etc)
*This event has a very difficult to distinguish source region, if you look very closely at S22 W38 just before 00:00 UT on the 10/05 it is possible to see a very small disturbance on the Sun, especially in 304 Angstroms. (Hess)
* M. Temmer: clear on-disk signatures - movie from SDO - are visible. It is a "silent" CME, hard to catch for space weather forecasters, but not a "stealth" in sense of no solar surface signatures at all.
http://sdowww.lmsal.com/sdomedia/SunInTime/2012/10/04/daily_211-193-171.mov [October 4, 15UT, central south]
*C. Moestl: looking at the whole October 4 SDO movie, there are also two other minor eruptions which I find very hard to distinguish from the 15 UT one (1. 7 UT, slightly west of disk center; 2. 0930 UT, south-east quadrant)
* timing - evolution from SDO FoV to coronagraph - is an issue and needs to be looked at in detail
* these eruptions are also visible in the SWAP data (http://proba2.oma.be/), including another minor one at 14h UT in the south-east quadrant (A. Devos)

=Image Data=
==In-Situ Data==
A combination of SWEPAM and MAG data from the ACE Satellite: 
[[File:plot_sw_mag_plasma_2012100700.png|350px]]
[[File:plot_sw_mag_2012100700.png|400px]]
[[File:plot_sw_vel_2012100700.png|350px]] 
The blue lines are an approximation of the CME cloud and the red line denotes the shock.

==Jmaps==
Jmaps from STEREO A and B along the CME leading edge position angle 

[[File:jmapA20101005.jpg|500px]]
[[File:jmapB20101005.jpg|500px]]

 

=Video Data=
[http://solar.gmu.edu/wiki/upload/phess4/aia3041005.avi AIA 304 Running Difference Movie] 
[http://solar.gmu.edu/wiki/upload/phess4/aia1931005.avi AIA 195 Running Difference Movie] 
[http://solar.gmu.edu/wiki/upload/phess4/euvi1005.avi STEREO EUVIA 304] 
[http://solar.gmu.edu/wiki/upload/phess4/cor2A1005_good.avi STEREO COR2A] 
[http://solar.gmu.edu/wiki/upload/phess4/cor2B1005_good.avi STEREO COR2B] 
[http://solar.gmu.edu/wiki/upload/phess4/hi1A1005.avi STEREO HI1A] 
[http://solar.gmu.edu/wiki/upload/phess4/hi1b1005.avi STEREO HI1B] 
[http://solar.gmu.edu/wiki/upload/phess4/hi2A1005.avi STEREO HI2A] 
[http://solar.gmu.edu/wiki/upload/phess4/hi2b1005.avi STEREO HI2B] 
[http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_movie.mp4 PROBA2 SWAPP 174] 
[http://solar.gmu.edu/wiki/upload/Adevos/20121004_swap_diff.mp4 PROBA2 SWAPP 174 Difference Movie] 

=References=