22.214.171.124 Energy and mass flux in the corona. Loss in form of conduction, radiation, gravitational enthalpy, and kinetic energy fluxes into the accelerating solar wind plasma.
We don't know what this goal is about. To be understood.
Operational requirements table:
YES / NO / Not required / MAYBE / GOOD TO HAVE / NUMBERS
|Duration of the observations||2 hours|
SPICE for 2 hours
EUI could support for half of it
|High latitude||Good to have||Low and high latitude|
|Solar cycle dependence||Yes|
|Linkage science||Good to have||A few hours of connected observations.|
|Far side observations||No|
|SPP||Good to have|
|Instruments||EUI, PHI, METIS, SPICE|
- SWA, SWA Normal Mode, A few hours of connected observations, other instruments: ALL.
- MAG: MAG Normal Mode.
- EUI, EUI synoptic mode (S). Modes Q (EUI Quiet Sun mode (Q)), C (EUI Coronal hole mode (C)) and A (EUI Active Region mode (A)) with min observation time 1h ( ? ). HRI Ly-alpha 5 s? for 2 hours (that's a lot) , 174 1 min (FSI 304 with same cadence ). Other instruments: SPICE.
SoloHI Normal mode
- Target: Quiet Sun, Active Regions, Coronal Holes
- Observing mode: Dynamics, Waves, 30” Wide Movie
- Slit: 2” for Dynamics, 4” for Waves, 30” for Wide Movie
- Exposure time/cadence and number of X positions: 5 s, X=128 for Dynamics; 5 s, X=720 for Waves; 5 s, X=120 for 30” Wide Movie (Fix Mirror for Waves and 30” Wide Movie, time series, multiple images)
Field of View: 4’×11’ for Dynamics, 48” ×11’ for Waves; 60” ×14” for 30” Wide MovieSame as for the previous one, see 126.96.36.199
- Number of repetitions of the study: 10 for Dynamics followed by 5 for Waves and 1 for 30” Wide Movie
- Observation time: 1.8 hours for Dynamics (0.2 hours per study), Wide movie 0.175 hours
- Key SPICE lines to be included: H I 1025 Å, C III 977 Å, O VI 1032 Å, Ne VIII 770 Å, Mg IX 706 Å, Si XII 520 Å (x2) – 10 lines (4 profiles and 6 intensities) for Dynamics; C III 977 Å, O VI 1032 Å, Ne VIII 770 Å- 3 lines for Waves; C III 977 Å, O VI 1032 Å – 1 or 2 line for 30” Wide Movie
- Observing window preference: High latitude when possible. Perihelion is good for high resolution.
- Other instruments: EUI/FSI and HRI for context imaging; PHI for magnetic field structure; METIS for solar wind mapping.
- 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.
- Possible binning on Y direction (groups of 4 pixels)
FDT medium resolution data
1024 x 1024
Ic, vLOS, B
PHI operating mode
- Measurement of the solar wind outflow velocity gradient in the outer corona, to localise regions of energy deposition, via Doppler dimming of the HI Lyα intensity in the field of view 1.5-2.9 degrees. Measurement of the magnetic field topology through the global corona configuration. Measurements of the brightness fluctuation spectra.
- Global maps of outflow velocity in corona.
- Global maps of the electron density in corona/coronal configuration.
- Brightness fluctuation spectra.
- WIND (min. obs time 2 hr, data volume ≤ 300 Mb)
- MAGTOP (min. obs time 2 hr, data volume ≤ 480 Mb)
- FLUCTS (min. obs time 1 hr, data volume ~ 2 Gb) at perihelion.
- Other instruments: PHI, EUI, SPICE, STIX.
- All instruments.
- A few hours of connected observations.