R_FULL_HRES_HCAD_Density-Fluctuations

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 40mins at 20s cadence)

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)
+ lower cadence during the rest of the window: several days min to observe the lower freq
duration: preferred to have it also 8h in the other 2 RSwindows

EUI

FSI Synoptic mode (S)

Deep exposures

Long exposures needed to get good SNR where it overlaps with Metis

PHI

 PHI_synoptic_FDT_4 

 6-hr cadence

1024 x 1024

I_c, B, γ, φ

for context

SPICE

(optional)

SPICE currently proposes to use either SPICE Limb mode or SPICE Dynamics, depending on the target.

Limb:

• Slit: 4"
• Exposure time: 5 s
• X positions: 224
• FoV: 15' x 11'
• Nº repeats: 10
• Observation time:
  • 18 mins per study
  • 3.2 hours total.

Active region (SPICE Dynamics) :

• Slit: 4"
• Exposure time: 60 s
• X positions: 128
• FoV: 8.5' x 11'
• Nº repeats: 1?
• Observation time: 2.1 hours

• Limb active region target best if present. Cannot participate if Metis is observing, so not modelled for now.

• If at limb: 224 positions of 60-s exposures, so lasting 4 hours; otherwise, the duration is as long as Metis requires.

Lines for SPICE Limb mode:

• H I 1025 Å,

• C III 977 Å,

• O VI 1032 Å,

• Ne VIII 770 Å,

• Mg IX 706 Å,

• Si XII 520 Å (2nd order) 

– 3 profiles and 3 intensities.

Lines for SPICE Dynamics:

• 4 profiles and 6 intensities.

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?