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YZ: Also linked to 1.1.2.2 Does slow and intermediate solar wind originate from coronal loops outside of coronal holes? 

(To be merged with 1.1.2.2 after the LTP planning exercise during SOWG#8.)


Meeting notes:

 

boundary crossing is the event we want to catch both IS and RS
model gives us a first rough idea on when we will cross the open/closed boundary in situ and when this plasma should have left the sun
eui/hri goes in high cadence observation well before the estimated crossing and well after: at 1min cadence  ~10hrs of data can be stored internally
when internal buffer is full, EUI stops
LL data are checked to see whether we see the boundary - updates if necessary
MAG LL data are checked to find the boundary crossing - wind speed gives us estimate when the wind left the sun (only up to source surface probably)
models can be compared with these observations
we need phi for context for data analysis 

 

extra idea: it would be great to observe the same boundary when it appears on the limb (both limbs?) with FSI and metis

 

Operational requirements table: 

 

Requirement
YES / NO / Not required / MAYBE / GOOD TO HAVE / NUMBERS
Remarks
Duration of the observationsA few days. 
PerihelionYes 
RS windowYes 
High latitudeYesLow and high latitude.
Solar cycle dependenceYes 
Radial dependenceNo 
Linkage scienceYesFor its relation to the slow wind.
Multiple orbitsYes 
Far side observationsNo 
Earth observationsGood to have. 
EMC QuietNo 
SPPGood to have. 
InstrumentsSoloHI, EUI, PHI, METIS, SPICE

RS only.

 

Required observations:

  • SoloHI: Contribute (mode: synoptic+shock+turbulence), no min. obs time, all distances.
  • EUIEUI synoptic mode (S). FSI 304, long duration, intermediate cadence 10 min. 
  • SPICE
    • Target:Coronal holes, coronal hole boundaries, quiet Sun, active regions
    • Observing mode: Composition mapping (with possibility to measure Doppler velocities) and possible mosaic for connectivity
    • Slit: 6” or 30” (for faster maps which the max FOV)

    • Exposure time/cadence and number of X positions: 180 s, X=160 or X=32
    • Field of View: 16’×11’ (with the 6” slit), 16’×14’ (with the 30” slit)
    • Number of repetitions of the study: 2 (using the 6” slit) or 10 (using the 30” slit)
    • Observation time: 16 hours (8 hours per study using the 6” slit or 1.6 hours per study using the 30” slit)
    • Key SPICE lines to be included: Ne VIII 770 Å, Ne VIII 780 Å, Mg IX 706 Å, O II 718 Å, O IV 787 Å, O V 760.4 Å, O V 761 Å, O VI 1032 Å, O VI 1037 Å, Ne VI 999 Å, Ne VI 1010 Å, Mg VIII 772 Å, Mg VIII 782 Å, C III 977 Å, Fe III 1017 Å - 2 profiles and 13 intensities or 4 profiles and 11 intensities (maximum of 15)
    • Observing window preference: High and low latitude, perihelion
    • Other instruments: EUI, PHI, SoloHI
    • 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.

       

  • PHI

    FDT medium-high  resolution data

    Requirement

    FOV [pixels]

    1024 x 1024 – 2048 x 2048

    Parameters

    Ic, B, γ, φ

    duration

    10 days

    cadence

    1/(10 min)

    N orbits

    4

    solar distance

    entire orbit

    PHI operating mode

    2

    co-ordination

    ?

    HRT high  resolution data

    Requirement

    FOV [pixels]

    2048 x 2048

    Parameters

    Ic, vLOS, B, γ, φ (interlaced with raw data)

    duration

    5 hours

    cadence

    1/(1 min)

    N orbits

    2

    solar distance

    perihelion, polar passage

    PHI operating mode

    0

    co-ordination

    ?

  • METIS: Measurement of the electron density through the polarised brightness in VL (580-640 nm) in the field of view 1.5-2.9 degrees to derive the evolution of the magnetic field topology from the global corona evolution in different time-scales.
    • Products:
      • Global maps of the electron density in corona/coronal configuration.
    • Modes:
      • MAGTOP (min. obs time 2 hr, data volume ≤ 480 Mb)
      • GLOBAL (min. obs time 2 hr, data volume ≤ 300 Mb)
        Repeated each half a day in one observation window.
    • Other instruments: PHI, EUI, SoloHI, MAG, SWA.

      Duration:

Other constraints: