Description of the objective:

In order to better understand the structure of CMEs, we have to explore the following:

  •  Three-part structure: bright leading shell, dark cavity, bright core (Illing and Hundhausen, 1986; Plunkett et al., 2000).
  •  Presence of large-scale helical magnetic flux rope in the CME cavity (Vourlidas et al., 2013).
  •  Counter-streaming electrons observations as signatures of field lines tied at both ends to the Sun (Crooker and Owens, 2012).
  •  Electron heat flux dropouts as signatures of magnetic flux disconnection from the Sun (Crooker and Owens, 2012). 
  •  Longitudinal distribution of the emitted plasma and detection of geoeffective events.

Relevant SOOPs:




      • Mostly IS Driven.
      • Target: Prominence, Active Regions.
      • Observing mode: CME Watch (with possibility to measure Doppler velocities).
      • Slit size: 6” 
      • Exposure time/cadence and number of X positions: 30 s, X=160 
      • Field of View: 16’×11’ 
      • Number of repetitions of the study: Number of repetitions driven by IS.
      • Observation time per day: The total observation time depends on the number of repetitions. 1.3 hours per study.
      • Key SPICE lines to be included: ?
      • Observing window preference: 
      • Other instruments: EUI, PHI, all IS.
      • Comments:  The choice of lines, and also the number of intensities and profiles, is flexible, although the sum of the intensities and profiles is constrained to a maximum (e.g 15 for composition mapping). While varying the number of intensities and profiles, within the maximum, has no effect on the duration of the study, it will have an effect on the telemetry.