08/05/2011 18:00:00 UTC - Revision history

Matemmer at 13:06, 31 August 2017

2017-08-31T13:06:11Z

2017-08-31T13:05:49Z

2017-08-30T07:00:11Z

‎Modeling and observations

2017-08-30T06:58:07Z

‎Video Data

2017-01-27T04:42:58Z

‎Comment Section

2013-07-01T23:03:01Z

2013-07-01T23:02:30Z

‎In-Situ Data

2013-06-19T08:55:47Z

‎Video Data

2013-06-03T00:50:36Z

2013-06-03T00:15:04Z

@@ Line 23: / Line 23: @@
 in the low corona.
-Two Figures (link below) illustrate evolution of the flux rope and CME plasma parameters at the first stage of their expansion obtained from MHD modeling and observations.
+Two Figures[https://drive.google.com/open?id=0B0-C__GSUWj2RDhrcTJqRWp1Y0k] illustrate evolution of the flux rope and CME plasma parameters at the first stage of their expansion obtained from MHD modeling and observations.
-[https://drive.google.com/open?id=0B0-C__GSUWj2RDhrcTJqRWp1Y0k]
 Reference: D. Rodkin F. Goryaev,  P. Pagano, G. Gibb, V. Slemzin, Y. Shugay, I. Veselovsky, D.H. Mackay
 “Origin and Ion Charge State Evolution of Solar Wind Transients during 4 – 7 August 2011” published in Solar Phys (2017), 292:90, DOI 10.1007/s11207-017-1109-0.
 =References=

@@ Line 23: / Line 23: @@
 in the low corona.
-Two Figures illustrate evolution of the flux rope and CME plasma parameters at the first stage of their expansion obtained from MHD modeling and observations.
+Two Figures (link below) illustrate evolution of the flux rope and CME plasma parameters at the first stage of their expansion obtained from MHD modeling and observations.
+[https://drive.google.com/open?id=0B0-C__GSUWj2RDhrcTJqRWp1Y0k]
 Reference: D. Rodkin F. Goryaev,  P. Pagano, G. Gibb, V. Slemzin, Y. Shugay, I. Veselovsky, D.H. Mackay
 “Origin and Ion Charge State Evolution of Solar Wind Transients during 4 – 7 August 2011” published in Solar Phys (2017), 292:90, DOI 10.1007/s11207-017-1109-0.
 =References=

@@ Line 12: / Line 12: @@
 The blue lines are an approximation of the CME cloud and the red line denotes the shock.
-=Modeling and observations=
+=Remote observations and modeling results =
 =References=

@@ Line 12: / Line 12: @@
 The blue lines are an approximation of the CME cloud and the red line denotes the shock.
-=Video Data=
+=Modeling and observations=
 =References=

@@ Line 2: / Line 2: @@
 *A "big" event of having everything: halo CME in C2, halo CME in COR2 A, M9-class flare, strong waves in coronal images
 *In-situ: only show shock structure; the CME ejectum might have missed the Earth
+*The marks on the GMU plots are wrong. This is not an MC event. The starting and ending times of MC should be removed (Jie Zhang 01/26/2017)
 =Image Data=
 ==In-Situ Data==

← Older revision	Revision as of 23:03, 1 July 2013
(No difference)

@@ Line 5: / Line 5: @@
 =Image Data=
 ==In-Situ Data==
-<pre style="color: red">  The following plots need to be updated. Timings are wrong(Jie). </pre>
-A combination of SWEPAM and MAG data from the ACE Satellite: <br />
+[[File:plot_sw_mag_plasma_2011080500.png|350px]]
-[[File:plot_sw_mag_plasma_2011080300.png|350px]]
+[[File:plot_sw_mag_2011080500.png|400px]]
-[[File:plot_sw_mag_2011080300.png|400px]]
+[[File:plot_sw_vel_2011080500.png|350px]] <br />
 The blue lines are an approximation of the CME cloud and the red line denotes the shock.