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Proposed SOOP Coordinators

C. Owen, Hardi Peter, Tim Horbury, Pradeep Chitta (Obj 4), D. Spadaro, A. Giunta, L. Harra, D. Baker


Try to catch with Remote Sensing instruments the dynamics at a open-closed field boundary which will then be crossed in situ. High resolution RS observations required to catch dynamics. This SOOP will in general need specific target pointing or target tracking unless the SC is far enough from the Sun to catch.

Default SOOP duration: 3 days

Pointing requirements: Off-pointing: specific target pointing or target tracking 

Triggers: only IS triggers enabled TBC

See SOOP 2 defined for SOWG8 planning exercise.

EPDclose mode + scheduled/triggered burst


normal + scheduled/triggered burst
RPWnormal + scheduled/triggered burstselective downlink useful
SWAnormal + scheduled/triggered burst
SPICEcombination SPICE Dynamics & SPICE Composition Mapping rasters

Raster area should be optimized to make sure open-closed field boundary is captured

Line choices optimized for type of target

Use observation called SPICE_WIND_CONNECT in modelling.
(See SPICE Pseudo-observations for SOOPs)


EUV & LYA Coronal hole modes (C) (uses HRI) at 1min cadence

FSI Synoptic mode (S) throughout

If TM is limited, varying priority schema can be used to keep HRI data manageable

Regularly spaced HRT data at medium to high resolution
e.g. PHI_magnetograph_HRT_2 (600s cadence default)  

+ regular PHI Full-disk Precursors

PHI LL magnetograms needed throughout.
Note that 1 hour cadence can suffice for interchange reconnection at high resolution. 

Processing after the RSW: PHI could focus downlink on the most interesting periods, as inferred from other LL data


MAGTOP or GLOBAL (see METIS standard modes) for context
and linkage of solar wind source regions to SC 

modelled as GLOBAL with default settings

Only applicable if beyond ~0.5AU during target tracking
SoloHIContext via SoloHI synoptic modesModel for now as HI_SYN_NEAR
STIXSTX_NORMALnot strictly needed for SOOP although context is appreciated
SAP objectiveTargetDurationOpportunity/Orbital configuration

Operational constraints 

Additional comments Does slow and intermediate solar wind originate from coronal loops outside of coronal holes? coronal loops outside of coronal holesfew days
  • near perihelion for resolution & better linkage conditions
  • different phases of solar cycle
  • radial alignment with SPP is a plus
  • it may be worthwhile to map around the whole AR to have higher chance of being connected
  • EMC quiet for connectivity

radial alignment with SPP is a plus Study fast plasma flows from the edges of solar active regions discovered with Hinode/EISedges of solar active regions - at most likely ballistic connection pointfew hours 
  • radial alignment with SPP is a plus
  • fast flows require high cadence observations (mainly SPICE and HRI?)
radial alignment with SPP is a plus Interchange reconnection between open and closed field lines and its role in slow wind generation

Open-Closed field line boundaries (near ballistic connection point):

  • CH boundaries
  • AR edges close to low-latitude open field
  • Intermediate areas of quiet Sun

Target tracking

~1 RSW (10 days)
  • to be studied for CHs in different locations (high vs low latitudes)
  • different opportunities along the orbit: high-latitude windows + perihelion
  • to be studied in different solar cycle phases
  • Earth view before the observations would be asset to use modelling to define best target
  • radial alignment with SPP is a plus
  • During RSW
  • pre-window synoptics needed for target choice
  • VSTP updates needed for target tracking
  • EMC quiet for connectivity
radial alignment with SPP is a plus Magnetic reconnection in the chromosphere, the transition region and the corona

Quiet Sun at various latitudes.several dayslow + high latitue, to be repeated along the cycle
  • during RSW
  • feature tracking

Only PHI, EUI/HRI and SPICE really necessary for this goal.

PHI/HRT mode 2 with 5-10 min cadence, 5 quantities and no binning

EUI/HRT follows cadence of PHI

To be discussed whether any of the following can be linked: Fine structures in the photosphere (Full characterization of photospheric magnetic fields) What is the distribution of the open magnetic flux? Detect and characterise waves in closed and open structures 

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  1. Anonymous

    (Andreas Lagg): This SOOP also covers the scientific plan proposed by Hardi Peter: "Solar wind variations on supergranular scales"

  2. SOOP ID in SOOP Kitchen = LS2