Latest revision as of 23:20, 8 October 2016

Comment Section

Perhaps due to the location of the spacecraft, I cannot see anything in STEREO to cause the ICME. I also see no significant Halo CMEs in LASCO during the days leading up to the in-situ signature. The Ying Liu paper listed in the reference section dealt only with the in-situ data, so I am not sure about the CME connection for this event. (Hess)
Three density peaks seemed to correspond to (1) sector boundary, (2) small ejecta, and (3) CIR interface, respectively (Jie Zhang)

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

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

compression of the magnetic cloud through a high speed stream (Rouillard et al. paper)
Liu, Y., Luhmann, J. G., Huttunen, K. E. J., Lin, R. P., Bale, S. D., Russell, C. T., & Galvin, A. B. (2008). Reconstruction of the 2007 May 22 Magnetic Cloud: How Much Can We Trust the Flux-Rope Geometry of CMEs? Astrophysical Journal, 677(2), L133–L136. doi:10.1086/587839

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 =Comment Section=
+*Perhaps due to the location of the spacecraft, I cannot see anything in STEREO to cause the ICME. I also see no significant Halo CMEs in LASCO during the days leading up to the in-situ signature. The Ying Liu paper listed in the reference section dealt only with the in-situ data, so I am not sure about the CME connection for this event. (Hess)
+*Three density peaks seemed to correspond to (1) sector boundary, (2) small ejecta, and (3) CIR interface, respectively (Jie Zhang)
 =Image Data=
 ==In-Situ Data==
 A combination of SWEPAM and MAG data from the ACE Satellite: <br />
+[[File:plot_sw_mag_plasma_2007052000.png|350px]]
+[[File:plot_sw_mag_2007052000.png|400px]]
+[[File:plot_sw_vel_2007052000.png|350px]] <br />
 The blue lines are an approximation of the CME cloud and the red line denotes the shock.