Proposed SOOP Coordinators
D. Spadaro, A. Vourlidas, D. Berghmans, A. Giunta
Study of density fluctuations in the extended corona as a function of the outflow velocity of the solar wind while evolving in the heliosphere. If SPICE participates, will need to have limb pointing for a period of time, then return to disc centre for the full-Sun instruments.
Default SOOP duration: 8 hours (but necessary to plan some runs with a definitely longer duration, up to 24-30 hours).
Pointing requirements: may require offpointing (e.g. limb)
Triggers: only IS triggers enabled
|Long exposures needed to get good SNR where it overlaps with Metis|
FLUCTS for 1 hour:
(20 mins of: 60 x 1s DIT + 10mins processing x2
then MAGTOP (5 to 20 mins cadence)
Extra processing time is only needed at 1s cadence - 60 images can be stored and queend for processing
primary at perihelion: METIS SNR for 1s cadence + near corotation (8hours) (latitude changes not a big problem if ~1degree or less)
1024 x 1024
Ic, B, γ, φ
Contributes with synoptic+shock+turbulence
modelled as 50% HI_SHOCK_PER + 50% HI_SYN_NEAR
|Seems like this could be a little better defined.|
Active region (SPICE Dynamics) :
Lines for SPICE Limb mode:
– 3 profiles and 3 intensities.
(e.g., orbital requirements, solar cycle phase, quadrature ...)
|188.8.131.52 Study of density fluctuations in the extended corona as a function of the outflow velocity of the solar wind while evolving in the heliosphere||Disc-centre to observe whole corona (except when SPICE observes at limb)||8 hours x 3|
1 8-hour observation in each RSW of an orbit
Good to have SPP in quadrature to observe the fluctuations in-situ.
|184.108.40.206 Energy and mass flux in the corona.|
|220.127.116.11 Determine where energy is deposited in the solar wind|
|18.104.22.168 What is the nature and origin of waves, turbulence and small-scale structures?|
|1.3.2 How is turbulent energy dissipated and how does turbulence evolve within the heliosphere?|