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Comment: Updates following inputs

General description

This SOOP is designed to let the high-resolution RS observations cover a wider area than normal, in particular the SPICE FOV


and is to be used


with a mosaic of pointings



The main goal is to link the source region on the Sun with the in situ measurements at the spacecraft, using composition maps (FIP bias maps) and comparing them with the composition measured in situ.


Default SOOP duration: 50 hours (minimum 48 hours).

Pointing requirements: mosaic of


Triggers: only IS triggers enabled



Observations requirement (baseline)

SPICE (leads)
  • Main study: SPICE Composition
Mapping (30mins per map)Slit:  4’’or 6”
  • map (3 - 8 hours: total duration depending on the exposure time, the available FOV according to the orbit conditions and the S/C constraints).
  • Supporting study: Spectral Atlas

Slit:  4’’ slit

Exposure time:

180 s
  • number of X positions = 10 (inferred, to maintain 30 minute cadence)
  • Field of View: 1.2 x 11’depending on step size chosen – i.e., not the same as the slit width – this could cover a larger region

    60 s, 90 s or 120 s according to the S/C constraints for the main study; 60 s for Spectral Atlas

    FOV: 20.2'×30' - 29'×30' depending on S/C constraints for the main study.

    Number of repetitions of the study:

    6 (

    usually one at each


    pointing, but also depends on S/C constraints.

    Observation time:

    6.4 hours

    Mosaic of 6 positions would take bit more than 3 hours

    Lines for SPICE Composition Mapping (from Does slow and intermediate solar wind originate from coronal loops outside of coronal holes?) :

    – 15 lines (2 profiles+ 13 intensities)

    • Ne VIII 770 Å,

    • Ne VIII 780 Å,

    • Mg IX 706 Å,

    • O II 718 Å,

    • O IV 787 Å,

    • O V 760 Å,

    • O V 761 Å,

    • O VI 1032 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

    • Si II 992 Å

    N.B. This line list for SPICE Composition Mapping is similar to that of L_BOTH_HRES_LCAD_CH-Boundary-Expansion, except for O VI 1037 (removed) and Si II 992 (added).


    PHI_magnetograph_FDT/HRT_2 with HRT, 15 mins cadence2 PHI/HRT datasets per SPICE map

    50 hours (minimum 48 hours) to reduce the constraints due to S/C.

    Main spectral line list (profiles):

    • O III 70.3 nm multiplet
    • Mg IX 70.6 nm
    • S IV 74.8 nm (if exp.time=90 s or 120 s)
    • Mg IX 74.9 nm (if exp.time=90 s or 120 s)
    • S IV 75.0 nm
    • N IV 76.5 nm
    • Ne VIII 77.0 nm
    • Mg VIII 77.2 nm
    • S V 78.6 nm
    • O IV 78.7 nm
    • N III 99.1 nm (if exp.time=90 s or 120 s)
    • C III 97.7 nm
    • O VI 103.2 nm.

    For the Spectral Atlas the full spectrum is available, but the FOV is much smaller than the main Composition map study.


    EUV & LYA Coronal hole modes (C) with HRI, 10-15 mins cadence

    FSI Synoptic mode (S) with FSI

    2-3 HRI images per SPICE map


    PHI_magnetograph_FDT/HRT_2 with HRT, 15 mins cadence

    SoloHI Synoptic program

    modelled as HI_SYN_NEAR

    cadences adapted to applicable sun distance and TM corridor
    STIXSTIX Normal Mode
    Metiswill generally be SAFE+door closed, due to off-pointing mosaic.
    IF far enough from Sun: METIS standard modes for context for connection

    EPDNormal Mode
    MAGNormal Mode
    RPWDetection ModeBurst Triggers Active
    SWANormal Mode

    Science objectives


    SAP objectiveTargetDurationOpportunity
    (e.g., orbital requirements, solar cycle phase, quadrature ...)

    Operational constraints 

    Additional comments Trace streamer blobs and other structures through the outer corona and the heliosphere.N-S mosaic Mosaic centred on most likely connection point3 hrs 50 hours + slews for mosaic of 6 positions (30mins dwell timeabout 8 hours per position)RSwindow -

    Preferred quadrature with Earth



    SoloHI images Earth-directed blobs, Earth images blobs that will hit Solar Orbiter

    Daily N-S mosaic driven by SPICE composition maps: 6 positions, 30 mins dwell time at each position

    SWA/HIS is needed.

    WOLs and PASS

    Pre-window observations with EUI and Metis desired for coronal context.

    radial Radial or quadrature alignment with SPP is a plus. Does slow and intermediate solar wind originate from coronal loops outside of coronal holes? coronal loops outside of coronal holesfew days

    AR boundaries/AR/ CH boundaries,

    50 hours + slews of 6 positions (about 8 hours per position)

    Near perihelion for resolution & better linkage conditions.


    Different phases of solar cycle

    Mosaic to map larger region (e.g. around AR)


    SWA/HIS is needed.

    Useful to run close to the L_SMALL_HRES_HCAD_Slow-Wind-Connection to have a longer tracking of the connection source plus context.

    WOLs and PASS.

    Modelling to find best candidate source regions


    Mosaic to map larger region for maximise the linkage with the source on the Sun.

    Radial or quadrature alignment with SPP is a plus. How does the heliospheric magnetic field disconnect from the Sun?

     AR boundaries/AR/ CH boundaries/ connection point

    50 hours + slews of 6 positions (about 8 hours per position)

    Any RS windows, but preferred either near perihelion for resolution or quadrature to allow Earth-based instruments support.

    SWA/HIS is needed.

    WOLs and PASS.

    Instances run / planned

    LTP6 (run):

    2022-03-02 to 03, 2022-03-30 to 31 (SOOP Coordinators: A. Giunta, N. Prado, D. Hassler

    LTP9 (run):

    2022-10-13 to 16 (SOOP Coordinators: A. Giunta)

    LTP11 (planned):

    2023-04-20 15 to 22 17 (SOOP Coordinators: A. Giunta, D. Hassler, N. Zambrana Prado).

    Science outcomes

    Ref of papers using the SOOP data