http://solar.gmu.edu/heliophysics/api.php?action=feedcontributions&feedformat=atom&user=Ymwang 2026-09-09T22:44:09Z User contributions MediaWiki 1.31.0 http://solar.gmu.edu/heliophysics/index.php?title=03/17/2015_04:00:00_UTC&diff=2581 2015-06-12T09:34:06Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *varSITI campaign event<br /> *Largest geomagnetic storm at Earth for solar cycle 24, this event registered a Dst peak of -228 nT. <br /> *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 ([[http://helioweather.net/archive/2015/03/cmes201503_vel3r2e1b.mp4]]) 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)<br /> *This super storm is produced through a combination of effects: (1) strong magnetic field in the sheath region (&gt; 25 nT at peak)) and ejecta (&gt;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).<br /> *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).<br /> *With the ElEvo model results for the March 15 04:00 UT CME shock propagation from Sun to Earth, I need a quite low value of gamma to get the Wind speed and arrival time right, which reflects that this CME did not seem to experience much drag during interplanetary propagation. If the CME apex is really about 40° away from the Earth (as indicated by the source region position), I think its very surprising that Earth is hit by the flux rope. I think this is only possible if the flux rope had a very low inclination to the ecliptic, or as said before that there was some interaction with the CME on March 14. Maybe the drag parameter is low because the CIR was pushing from behind, adding an additional force? (Christian Moestl)<br /> *For Christian's high inclination problem, I think that an explanation is the deflection. My theory proposed that fast CMEs deflect toward east and slow CMEs deflect toward west (Wang et al., JGR, 119, 5117, 2014). Also there are in situ signatures of such possible deflection. From fitting results of my velocity-modified flux rope model, we find there is significant propagation velocity of the CME at 1 AU which is perpendicular to the Sun-Earth line (in +y direction in GSE coordinates). (Yuming Wang)<br /> <br /> =Image Data=<br /> <br /> ==In-situ data==<br /> [[File:20150315_magplasma.png]] <br /> [[File:20150315_mag.png]] &lt;br&gt;<br /> *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)<br /> <br /> ==LASCO/Kanzelhöhe==<br /> Image collection of white light and chromospheric data, showing two disturbances and the partly erupted filament which is related to the CME producing AR:<br /> [link http://www.uni-graz.at/~temmerma/download/varsiti/20150315.pdf]<br /> <br /> ==GOES Plot==<br /> [[File:20150315_goes.png]]<br /> <br /> ==SOHO/LASO measurement==<br /> [[File:Hess_heights.png|700px]]<br /> *Height-Time plot based on SOHO/LASCO measurement<br /> [[File:Hess_velocity.png|700px]]<br /> *Velocity-Time plot from SOHO/LASCO H-T measurement<br /> *Height-Time measurement data from SOHO/LASCO: [[Hess_measurement.docx]]<br /> <br /> == Interplanetary Propagation ==<br /> Christian Möstl and Tanja Rollett:<br /> ElEvo results (parameters already tweaked so it matches Wind arrivals):<br /> shock arrival at Wind: March 17 03:50 UT<br /> arrival speed 665 km/s<br /> <br /> Wind observations (taken from the Wu et al. draft):<br /> shock arrival March 17 03:59 UT<br /> arrival speed of the sheath is 500- 600 km/s, about 100 km/s less than the ElEvo arrival speed. <br /> <br /> This model/plot can be adjusted very easily if you think the CME initial speed, direction and launch time should be different. <br /> <br /> initial CME parameters:<br /> inital speed at 15 Rs: 1120 km/s, at time 2015 March 15 04:00 UT, direction to Earth west 39°<br /> the speed was taken from Kevin Schenk real time email, consistent with Gopalswamy et al. proceeding; same for direction. Thus I assume that the source region position is similar to the CME direction. Because the flare happens inside the AR and there are no large coronal holes nearby, it should be relatively safe to assume this direction as the CME propagation direction. The asymmetric halo with more material to the west of the Sun also supports this. Other Parameters: background wind: 400 km/s, gamma: 0.1, ellipse aspect ratio 1.6, full width: 100° in heliospheric longitude.<br /> <br /> [[File:elevo_15_mar_2015_storm_small2.png]]<br /> <br /> =Video Data=<br /> [http://solar.gmu.edu/wiki/upload/phess4/201503171.gif AIA 171 movie] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/201503193.gif AIA 193 movie] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/201503304.gif AIA 304 movie] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/2015031600.gif AIA 1600 movie] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/201503hmi.gif HMI movie] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/201503c2.gif C2 movie] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/201503c3.gif C3 movie] &lt;br&gt;<br /> <br /> =References=<br /> ElEvo model: Möstl et al. 2015 Nature Communications, open access: http://www.nature.com/ncomms/2015/150526/ncomms8135/full/ncomms8135.html</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2062 2014-04-18T09:49:47Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> ** 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)<br /> <br /> =Image Data=<br /> ==In-Situ Data from Wind==<br /> (Edited by Yuming Wang, 2014/04/18)<br /> <br /> Two ejecta are possible.<br /> <br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> ** The fitted coefficients of ejecta 1 are:<br /> *** B0 = 52.098665 nT<br /> *** R = 0.28131624 AU<br /> *** Theta = -45.039456 deg<br /> *** Phi = 150.04089 deg<br /> *** H = 1.0000000<br /> *** d = -0.88881733<br /> *** t_cen = 15-Jul-2012 17:57:21 UT<br /> *** v_x = -547.26224 km/s<br /> *** v_y = -200.49954 km/s<br /> *** v_z = -36.381346 km/s<br /> *** v_exp = 226.05119 km/s, [200.91822, 225.96896]<br /> <br /> ** The fitted coefficients of ejecta 2 are:<br /> *** B0 = 16.776497 nT<br /> *** R = 0.056126660 AU<br /> *** Theta = -16.776502 deg<br /> *** Phi = 332.51921 deg<br /> *** H = -1.0000000<br /> *** d = -0.81328377<br /> *** t_cen = 16-Jul-2012 20:41:59 UT<br /> *** v_x = -420.51633 km/s<br /> *** v_y = -20.269702 km/s<br /> *** v_z = 26.046412 km/s<br /> *** v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]<br /> <br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2061 2014-04-18T09:47:44Z

<p>Ymwang: /* In-Situ Data from Wind */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> <br /> =Image Data=<br /> ==In-Situ Data from Wind==<br /> (Edited by Yuming Wang, 2014/04/18)<br /> <br /> Two ejecta are possible.<br /> <br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> ** The fitted coefficients of ejecta 1 are:<br /> *** B0 = 52.098665 nT<br /> *** R = 0.28131624 AU<br /> *** Theta = -45.039456 deg<br /> *** Phi = 150.04089 deg<br /> *** H = 1.0000000<br /> *** d = -0.88881733<br /> *** t_cen = 15-Jul-2012 17:57:21 UT<br /> *** v_x = -547.26224 km/s<br /> *** v_y = -200.49954 km/s<br /> *** v_z = -36.381346 km/s<br /> *** v_exp = 226.05119 km/s, [200.91822, 225.96896]<br /> <br /> ** The fitted coefficients of ejecta 2 are:<br /> *** B0 = 16.776497 nT<br /> *** R = 0.056126660 AU<br /> *** Theta = -16.776502 deg<br /> *** Phi = 332.51921 deg<br /> *** H = -1.0000000<br /> *** d = -0.81328377<br /> *** t_cen = 16-Jul-2012 20:41:59 UT<br /> *** v_x = -420.51633 km/s<br /> *** v_y = -20.269702 km/s<br /> *** v_z = 26.046412 km/s<br /> *** v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]<br /> <br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2060 2014-04-18T09:47:31Z

<p>Ymwang: /* In-Situ Data from Wind */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> <br /> =Image Data=<br /> ==In-Situ Data from Wind==<br /> (Edited by Yuming Wang, 2014/04/18)<br /> Two ejecta are possible.<br /> <br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> ** The fitted coefficients of ejecta 1 are:<br /> *** B0 = 52.098665 nT<br /> *** R = 0.28131624 AU<br /> *** Theta = -45.039456 deg<br /> *** Phi = 150.04089 deg<br /> *** H = 1.0000000<br /> *** d = -0.88881733<br /> *** t_cen = 15-Jul-2012 17:57:21 UT<br /> *** v_x = -547.26224 km/s<br /> *** v_y = -200.49954 km/s<br /> *** v_z = -36.381346 km/s<br /> *** v_exp = 226.05119 km/s, [200.91822, 225.96896]<br /> <br /> ** The fitted coefficients of ejecta 2 are:<br /> *** B0 = 16.776497 nT<br /> *** R = 0.056126660 AU<br /> *** Theta = -16.776502 deg<br /> *** Phi = 332.51921 deg<br /> *** H = -1.0000000<br /> *** d = -0.81328377<br /> *** t_cen = 16-Jul-2012 20:41:59 UT<br /> *** v_x = -420.51633 km/s<br /> *** v_y = -20.269702 km/s<br /> *** v_z = 26.046412 km/s<br /> *** v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]<br /> <br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2059 2014-04-18T09:47:15Z

<p>Ymwang: /* Image Data */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> <br /> =Image Data=<br /> ==In-Situ Data from Wind==<br /> (Edited by Yuming Wang, 2014/04/18)<br /> Two ejecta are possible.<br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> ** The fitted coefficients of ejecta 1 are:<br /> *** B0 = 52.098665 nT<br /> *** R = 0.28131624 AU<br /> *** Theta = -45.039456 deg<br /> *** Phi = 150.04089 deg<br /> *** H = 1.0000000<br /> *** d = -0.88881733<br /> *** t_cen = 15-Jul-2012 17:57:21 UT<br /> *** v_x = -547.26224 km/s<br /> *** v_y = -200.49954 km/s<br /> *** v_z = -36.381346 km/s<br /> *** v_exp = 226.05119 km/s, [200.91822, 225.96896]<br /> <br /> ** The fitted coefficients of ejecta 2 are:<br /> *** B0 = 16.776497 nT<br /> *** R = 0.056126660 AU<br /> *** Theta = -16.776502 deg<br /> *** Phi = 332.51921 deg<br /> *** H = -1.0000000<br /> *** d = -0.81328377<br /> *** t_cen = 16-Jul-2012 20:41:59 UT<br /> *** v_x = -420.51633 km/s<br /> *** v_y = -20.269702 km/s<br /> *** v_z = 26.046412 km/s<br /> *** v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]<br /> <br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2058 2014-04-18T09:45:32Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2057 2014-04-18T09:43:46Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> ** The fitted coefficients of ejecta 1 are:<br /> *** B0 = 52.098665 nT<br /> *** R = 0.28131624 AU<br /> *** Theta = -45.039456 deg<br /> *** Phi = 150.04089 deg<br /> *** H = 1.0000000<br /> *** d = -0.88881733<br /> *** t_cen = 15-Jul-2012 17:57:21 UT<br /> *** v_x = -547.26224 km/s<br /> *** v_y = -200.49954 km/s<br /> *** v_z = -36.381346 km/s<br /> *** v_exp = 226.05119 km/s, [200.91822, 225.96896]<br /> <br /> ** The fitted coefficients of ejecta 2 are:<br /> *** B0 = 16.776497 nT<br /> *** R = 0.056126660 AU<br /> *** Theta = -16.776502 deg<br /> *** Phi = 332.51921 deg<br /> *** H = -1.0000000<br /> *** d = -0.81328377<br /> *** t_cen = 16-Jul-2012 20:41:59 UT<br /> *** v_x = -420.51633 km/s<br /> *** v_y = -20.269702 km/s<br /> *** v_z = 26.046412 km/s<br /> *** v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2056 2014-04-18T09:42:03Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> %% The fitted coefficients of ejecta 1 are:<br /> %% B0 = 52.098665 nT<br /> %% R = 0.28131624 AU<br /> %% Theta = -45.039456 deg<br /> %% Phi = 150.04089 deg<br /> %% H = 1.0000000<br /> %% d = -0.88881733<br /> %% t_cen = 15-Jul-2012 17:57:21 UT<br /> %% v_x = -547.26224 km/s<br /> %% v_y = -200.49954 km/s<br /> %% v_z = -36.381346 km/s<br /> %% v_exp = 226.05119 km/s, [200.91822, 225.96896]<br /> <br /> %% The fitted coefficients of ejecta 2 are:<br /> %% B0 = 16.776497 nT<br /> %% R = 0.056126660 AU<br /> %% Theta = -16.776502 deg<br /> %% Phi = 332.51921 deg<br /> %% H = -1.0000000<br /> %% d = -0.81328377<br /> %% t_cen = 16-Jul-2012 20:41:59 UT<br /> %% v_x = -420.51633 km/s<br /> %% v_y = -20.269702 km/s<br /> %% v_z = 26.046412 km/s<br /> %% v_exp = 9.9780682 km/s, [8.1150009, 9.9576277]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2055 2014-04-18T09:40:24Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overall.jpg|300px]]<br /> [[File:ejectal.jpg|300px]]<br /> [[File:ejecta2.jpg|300px]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=File:Ejecta2.jpg&diff=2054 2014-04-18T09:39:59Z

<p>Ymwang: </p> <hr /> <div></div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=File:Ejectal.jpg&diff=2053 2014-04-18T09:37:44Z

<p>Ymwang: </p> <hr /> <div></div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2052 2014-04-18T09:37:26Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overall.jpg|200px]]<br /> [[File:ejectal.jpg|200px]]<br /> [[File:ejecta2.jpg|200px]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=File:Overall.jpg&diff=2051 2014-04-18T09:36:21Z

<p>Ymwang: </p> <hr /> <div></div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2050 2014-04-18T09:35:26Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overall.jpg|200px]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2049 2014-04-18T09:33:01Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:all.png|200px]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2048 2014-04-18T09:32:39Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:all.png|200px|thumb]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=File:All.png&diff=2047 2014-04-18T09:31:00Z

<p>Ymwang: </p> <hr /> <div></div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2046 2014-04-18T09:28:40Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:all.png]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2045 2014-04-18T09:27:42Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overview.png]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2044 2014-04-18T09:27:12Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=File:Overview.png&diff=2043 2014-04-18T09:24:01Z

<p>Ymwang: </p> <hr /> <div></div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=07/14/2012_17:00:00_UTC&diff=2042 2014-04-18T09:23:13Z

<p>Ymwang: /* Comment Section */</p> <hr /> <div>=Comment Section=<br /> *A perfect CME-ICME chain event (J. Zhang)<br /> **classical ICME feature: shock + sheath + magnetic cloud<br /> **strong solar signature: X1 flare (S17W08); halo CME, fast and bright<br /> *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)<br /> *Time Line (2014/04/18, Jie Zhang)<br /> **07/12 15:37 UT: Flare onset; 0 hr<br /> **07/12 16:49 UT: Flare peak (X1.4, S13S03, AR1520); 1 hr 12 min<br /> **07/12 16:48 UT: CME first appear in C2; 1 hr 11 min<br /> **07/12 18:54 UT: CME at 20 Rs; 3 hr 17 min<br /> **07/13 00:49 UT: CME at 50 Rs; 9 hr 12 min<br /> **07/13 06:49 UT: CME at 80 Rs; 15 hr 12 min <br /> **07/14 17:00 UT: Shock arrival at 1 AU; 49 hr 23 min<br /> **07/15 06:00 UT: Magnetic Cloud arrival at 1 AU; 62 hr 23 min<br /> **07/15 19:00 UT: Peak time of Dst (-127 nT); 75 hr 23 min<br /> **07/17 14:00 UT: Magnetic Cloud end at 1 AU; 118 hr 23 min<br /> <br /> *04/17 Hefei Discussion<br /> **Insitu data and Flux rope fitting (2014/04/18, Yuming Wang)<br /> [[File:overview.png]]<br /> <br /> =Image Data=<br /> ==In-Situ Data==<br /> A combination of SWEPAM and MAG data from the ACE Satellite: &lt;br /&gt;<br /> [[File:plot_sw_mag_plasma_2012071400.png|350px]]<br /> [[File:plot_sw_mag_2012071400.png|400px]]<br /> [[File:plot_sw_vel_2012071400.png|350px]] &lt;br /&gt;<br /> The blue lines are an approximation of the CME cloud and the red line denotes the shock.&lt;br /&gt;<br /> <br /> &lt;br /&gt;<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. &lt;br /&gt;<br /> <br /> [[File:Data_july122012.png|500px]]<br /> &lt;br /&gt;<br /> <br /> == Heliospheric Imaging ==<br /> CME track observed in STEREO-A Jmap with SATPLOT software: (C. Moestl) &lt;br /&gt;<br /> [[File:satplot_jmap_july122012.png|400px]] &lt;br /&gt;<br /> results of geometrical modeling (C. Moestl): &lt;br /&gt;<br /> [[File:Geometry_12_july2012.jpeg‎|400px]] &lt;br /&gt;<br /> <br /> Jmaps along the CME leading edge position (about &lt;math&gt;7^{\circ}&lt;/math&gt; S of the ecliptic) from STEREO A and B<br /> [[File:20120712JmapA.png|500 px]] [[File:20120712JmapB.png|500 px]] &lt;br&gt;<br /> <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.<br /> <br /> [[File:20120712stack.png]] &lt;br&gt;<br /> <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 &lt;br&gt;<br /> <br /> ==Flare Data==<br /> *[[File:eve_flare_2012_07_12.pdf]] EVE and GOES flare profiles<br /> *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&amp;clip=1&amp;flare_id=2989]<br /> <br /> *GOES X-RAY FLUX<br /> [[File:20120712_goes.png|500px]]&lt;br /&gt;&lt;br /&gt;<br /> The GOES X-ray Flux of the flare associated with the event. The vertical line approximately denotes the flare peak time. &lt;br /&gt;<br /> <br /> =Video Data=<br /> ==SDO observations==<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_94.avi AIA-94]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_AIA_171.mp4 AIA-171] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/enif/aia_12072012_211.avi AIA-211]&lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/JieZhang/20120712_1600-1730_HMI_B.mp4 HMI B] &lt;br&gt;<br /> <br /> ==STEREO observations==<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2A.avi COR2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/cor2B.avi COR2B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi1Ard.avi HI1A] &lt;br&gt;<br /> phess4/hi1Brd.avi HI1B] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Ard.avi HI2A] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/phess4/hi2Brd.avi HI2B] &lt;br&gt;<br /> <br /> ==PROBA2 observations==<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_movie.mp4 PROBA2 SWAP 174] &lt;br&gt;<br /> [http://solar.gmu.edu/wiki/upload/Adevos/20120712_swap_diff.mp4 PROBA2 SWAP 174 Difference Movie] &lt;br&gt;<br /> <br /> =References=</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_ICME%5CCME_Lists&diff=1428 2013-06-18T10:48:19Z

<p>Ymwang: /* Individual User Lists */</p> <hr /> <div>==ISEST Master List==<br /> [[The ISEST Master CME List]] &lt;br&gt;<br /> <br /> <br /> ==Individual User Lists==<br /> [[GMU CME/ICME List]] &lt;br&gt;<br /> [http://www.srl.caltech.edu/ACE/ASC/DATA/level3/icmetable2.htm Richardson/Cane List]&lt;br&gt;<br /> [http://www-ssc.igpp.ucla.edu/~jlan/ACE/Level3/ICME_List_from_Lan_Jian.pdf Jian List (through 2009)] &lt;br&gt;<br /> [http://cdaw.gsfc.nasa.gov/CME_list/halo/halo.html CDAW Halo CME List] &lt;br&gt;<br /> [ftp://www.iki.rssi.ru/pub/omni/ RSSI List] &lt;br&gt;<br /> [http://www.uni-graz.at/~moestlc/events/chris_list_v1.htm Christian Moestl CME/ICME list 2008-2012] &lt;br&gt;<br /> [http://space.ustc.edu.cn/dreams/fhcmes/ STEP Group @ USTC: A list of full halo CMEs with de-projected parameters and associated ICMEs since 2007 March] &lt;br&gt;</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=The_ISEST_ICME%5CCME_Lists&diff=1427 2013-06-18T10:47:28Z

<p>Ymwang: /* Individual User Lists */</p> <hr /> <div>==ISEST Master List==<br /> [[The ISEST Master CME List]] &lt;br&gt;<br /> <br /> <br /> ==Individual User Lists==<br /> [[GMU CME/ICME List]] &lt;br&gt;<br /> [http://www.srl.caltech.edu/ACE/ASC/DATA/level3/icmetable2.htm Richardson/Cane List]&lt;br&gt;<br /> [http://www-ssc.igpp.ucla.edu/~jlan/ACE/Level3/ICME_List_from_Lan_Jian.pdf Jian List (through 2009)] &lt;br&gt;<br /> [http://cdaw.gsfc.nasa.gov/CME_list/halo/halo.html CDAW Halo CME List] &lt;br&gt;<br /> [ftp://www.iki.rssi.ru/pub/omni/ RSSI List] &lt;br&gt;<br /> [http://www.uni-graz.at/~moestlc/events/chris_list_v1.htm Christian Moestl CME/ICME list 2008-2012] &lt;br&gt;<br /> [http://space.ustc.edu.cn/dreams/fhcmes/ STEP Group @ USTC: A list of full halo CMEs with de-projected parameters and associated ICMEs] &lt;br&gt;</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1420 2013-06-18T10:40:32Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> The tasks in the coming year:<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> **Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> **Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> **Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> **GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> **Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, Chin-Chun Wu, ……<br /> *Models &amp; Methods:<br /> **CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1419 2013-06-18T10:40:13Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> The tasks in the coming year:<br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> **Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> **Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> **Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> **GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> **Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, Chin-Chun Wu, ……<br /> *Models &amp; Methods:<br /> **CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1418 2013-06-18T10:39:32Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> **Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> **Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> **Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> **GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> **Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, Chin-Chun Wu, ……<br /> *Models &amp; Methods:<br /> **CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1417 2013-06-18T10:38:16Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, ……<br /> *Models &amp; Methods:<br /> **CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1416 2013-06-18T10:37:52Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, ……<br /> *Models &amp; Methods:<br /> CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1415 2013-06-18T10:37:33Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, ……<br /> *Models &amp; Methods:<br /> CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1413 2013-06-18T10:35:20Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> *Which conditions, How significant, Physical mechanisms, ……<br /> *Participants:<br /> Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> *Models &amp; Methods:<br /> GCS model, Triangulation methods, spherical methods, ……<br /> <br /> 3.3 Addressing CME arrival<br /> *Compare models, input/output parameters, ……<br /> *Participants:<br /> Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, ……<br /> *Models &amp; Methods:<br /> CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1412 2013-06-18T10:34:23Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> 3.1 Addressing aerodynamics of ICMEs in IP space<br /> *Drag force/coefficient, external forces, internal forces, …<br /> *Participants:<br /> Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> *Models &amp; Methods:<br /> Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> 3.2 Addressing deflection of ICMEs’ propagation<br /> Which conditions, How significant, Physical mechanisms, ……<br /> Participants:<br /> Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> Models &amp; Methods:<br /> GCS model, Triangulation methods, spherical methods, ……<br /> <br /> (3) Addressing CME arrival<br /> Compare models, input/output parameters, ……<br /> Participants:<br /> Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, ……<br /> Models &amp; Methods:<br /> CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang http://solar.gmu.edu/heliophysics/index.php?title=Working_Group_2&diff=1411 2013-06-18T10:33:12Z

<p>Ymwang: /* Results of the Workshop and Future Plans/Collaborations */</p> <hr /> <div>Theory group led by Bojan Vrsnak (Croatia) and Yuming Wang (China)<br /> <br /> ----<br /> <br /> <br /> =='''Objectives'''==<br /> * Initiation of CMEs and their take-off dynamics (&quot;acceleration stage&quot;)<br /> <br /> * Heliospheric dynamics of ICMEs and evolution of their structure<br /> <br /> * Relationship between empirical, analytical, and numerical propagation models and comparison with observations; forecasting aspects<br /> <br /> * CME/ICME-associated phenomena (flares, shocks, SEPs, etc.)<br /> <br /> * Together with WG3, WG2 should provide a &quot;theoretical-background service&quot; to WG1 and WG2<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Scientific Questions'''==<br /> ===''Which mechanisms, processes, forces are governing the CME take-off and ICME propagation?'' ===<br /> 2.1.1 What is the role of the flare-associated reconnection?<br /> <br /> 2.1.2 What is the role of emerging flux and poloidal-flux injection?<br /> <br /> 2.1.3 How long the Lorentz force dominates over the aerodynamic drag<br /> <br /> 2.1.4 How the inductive effects affect the CME eruption and ICME propagation?<br /> <br /> 2.1.5 What is the role of the ICME/ambient-field reconnection?<br /> <br /> 2.1.6 How to measure the real mass of ICMEs?<br /> <br /> ----<br /> <br /> ===''How much variable ambient conditions affect ICMEs?''===<br /> 2.2.1 Which processes are involved in ICME-ICME interactions?<br /> <br /> 2.2.2 How ICME-ICME interactions affect the dynamics and structure of ICMEs?<br /> <br /> 2.2.3 How high-speed solar wind streams (corotating interacting regions) affect ICMEs?<br /> <br /> 2.2.4 How the ICME-driven shock forms and evolves in the decreasing Alfven-velocity environment?<br /> <br /> 2.2.5 How ambient solar wind exchanges momentum, energy and magnetic flux with ICMEs?<br /> <br /> 2.2.6 What is the morphological shape of an ICME?<br /> <br /> 2.2.7 How does the morphological shape change and evolve from the Sun to the Earth? <br /> <br /> ----<br /> <br /> ===''What is the state of the art in the ICME-arrival and ICME-geoeffectiveness forecasting?''===<br /> 2.3.1 What are forecasting-performances of various empirical, analytical, and numerical models?<br /> <br /> 2.3.2 How well models reproduce heliospheric kinematics of ICMEs?<br /> <br /> 2.3.3 What are the key model-input parameters?<br /> <br /> 2.3.4 What can be done regarding the geomagnetic-activity forecasting?<br /> <br /> 2.3.5 What processes determine the ICME Forbush-decrease effectiveness?<br /> <br /> ----<br /> <br /> ===''The CME-associated phenomena''===<br /> <br /> 2.4.1 What are the mechanisms of initiation and what is the nature of CME-driven coronal waves and shocks?<br /> <br /> 2.4.2 What is the role of flares in the initiation and acceleration of CMEs?<br /> <br /> 2.4.3 What can we learn from coronal dimmings?<br /> <br /> 2.4.4 How the associated phenomena (flares, waves, dimmings) can help in the space-weather forecasting? <br /> <br /> 2.4.5 How SEPs are accelerated by shocks and how they transport in heliosphere?<br /> <br /> ----<br /> <br /> ----<br /> <br /> =='''Results of the Workshop and Future Plans/Collaborations'''==<br /> <br /> (1) Addressing aerodynamics of ICMEs in IP space<br /> Drag force/coefficient, external forces, internal forces, …<br /> Participants:<br /> Bojan Vrsnak, Jie Zhang, Christian Moestl, Yuming Wang, Fang Shen, Valbona Kunkel, ……<br /> Models &amp; Methods:<br /> Drag model, flux rope model, Triangulation methods, spherical methods, ……<br /> <br /> (2) Addressing deflection of ICMEs’ propagation<br /> Which conditions, How significant, Physical mechanisms, ……<br /> Participants:<br /> Manuela Temmer, Chenglong Shen, Noe Lugaz, ……<br /> Models &amp; Methods:<br /> GCS model, Triangulation methods, spherical methods, ……<br /> <br /> (3) Addressing CME arrival<br /> Compare models, input/output parameters, ……<br /> Participants:<br /> Nandita Srivastava, Luciano Rodriguez, Philippe Lamy, Yuming Wang, Dusan Odstrcil, ……<br /> Models &amp; Methods:<br /> CME auto-detection methods, cone models, Drag model, ENLIL model, HAF model, WSA model, ……</div>

Ymwang