General description
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. However, a complete and detailed study of coronal density fluctuations requires a long temporal baseline (up to 24-30 hours).
Pointing requirements: may require offpointing (e.g. limb)
Triggers: only IS triggers enabled
Observations requirement (baseline)
Instrument | Mode | Comment |
---|---|---|
SoloHI (lead) | Contributes with synoptic+shock+turbulence modelled as 50% HI_SHOCK_PER + 50% HI_SYN_NEAR | disk center or stable pointing required. Fast cadence (1-min) radial subfields consisting of sums of multiple images. Note: The exposure used in LTP9 were too short to provide sufficient SNR at those distances. The program is revised and a new version will be used in LTP11 with higher exposures and slighlt longer cadence (6 min). |
Metis (lead) | 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) |
EUI | Deep exposures | Long exposures needed to get good SNR where it overlaps with Metis |
PHI | 6-hr cadence 1024 x 1024 Ic, B, γ, φ | for context |
SPICE (optional) | SPICE currently proposes to use either SPICE Limb mode or SPICE Dynamics, depending on the target. Limb:
Active region (SPICE Dynamics) :
|
Lines for SPICE Limb mode:
– 3 profiles and 3 intensities.
|
Science objectives
SAP objective | Target | Duration | Opportunity (e.g., orbital requirements, solar cycle phase, quadrature ...) | Operational constraints | Additional comments |
---|---|---|---|---|---|
1.1.2.4 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. | ||
1.2.1.2 Energy and mass flux in the corona. | |||||
1.2.2.1 Determine where energy is deposited in the solar wind | |||||
1.2.2.3 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? |
Instances run / planned, differences from the baseline observations
With respect to the baseline observations requirements, Metis added to the FLUCTS_TBF mode (duration 1 hr) total brightness (tB)
observations with cadence of 1-2 min and duration of several hours, during both LTP9 and LTP11.
LTP9
2022-10-12 to 13 (SOOP coordinators: Daniele Spadaro).
Note: No density fluctuation detected with sufficient SNR for science analysis.
LTP11
2023-04-12 to 14 (SOOP coordinators: Daniele Spadaro, Angelos Vourlidas)
Proposed SOOP Coordinators
D. Spadaro, A. Vourlidas, D. Berghmans, A. Giunta
1 Comment
Anik De Groof
SOOP ID in SOOP Kitchen = RF1