^^^ Figure 1: 20 days of data from the October 18 1995 magnetic cloud event, indicating approximate CME ejection time, radio storm, and Type III events. Postscipt version
^^^ Figure 2: Data from October 18 event, including electron data from the WIND 3D Plasma and Energetic Particle Experiment. The presence of the time-of-flight characteristics of the electrons (high energy arriving first, followed by lower energy) are assumed to correspond to closed connected field lines within the cloud, while the absence of this behavior is attributed to crossing a disconnected field line (see data just below the electron plots). Judging from the relative times of flight, he determines the approximate field line length, or starting point, of these groups of electrons. Postscipt version
^^^ Figure 3: Cartoon showing magnetic field lines corresponding to closed flux tubes and "disconnected" field lines, identified in Figure 2. Postscipt version
^^^ Figure 4: 6 day summary plot of in-situ plasma data from multiple experiments. The following data is shown:
Panel 1: Ion flux vs. Energy (Protons are in the lower band,
Alphas are occasionally resolved
at 2 times the proton energy)
Panels 2-4: Magnetic field Strength, theta and phi
Panels 5-9: (Red:SWE , Blue:3DP).
Panel 5: Solar Wind Proton Density (At high densities and low
temperatures the 3DP detector saturates. this has not been corrected for this plot.)
Panels 6-8: Solar Wind Flow Speed, Theta and Phi
Panel 9: Thermal Velocity over Flow speed.
Panel 10: Rough Alpha ratio. (very crude! not yet corrected)
Panel 11: Wave Intensity
Panel 12-14: Electron Pitch Angle distributions
Panel 15: Electron Flux opposite B
Panel 16: Electron Flux along B
Postscipt version