General description

Similar to L_SMALL_HRES_HCAD_Slow-Wind-Connection, but specifically targeted at overexpanded CH boundaries as slow wind sources, requiring a different PHI mode and SPICE observations.

This SOOP was explicitly created to address the science objective "Does slow wind originate from the over-expanded edges of coronal holes?" and does not currently cover any other sub-objectives. The similar SOOP SlowWind Connection addresses all other slow solar wind objectives and mainly involves RS instruments observing the solar disk, even at high spatial resolution.   

Default SOOP duration: 1 day

Pointing requirements: Off-pointing (for SPICE Composition Mapping and Dynamics), combined with disk-centre.  

Triggers: only IS triggers enabled 

Observations requirement (baseline)


InstrumentModeComment
EPDN/A

MAG

normal + scheduled/triggered burst
RPWnormal + scheduled/triggered burst
SWAnormal + scheduled/triggered burst
SPICE

SPICE Dynamics (on 1 day), 4–6 rasters, depending on structure. (Modelling as 6 rasters = 1 hour )

3–4 subsequent days of regular observations: SPICE Composition Mapping interleaved with SPICE Dynamics

Full north-south raster only needed for extended coronal holes. Otherwise point at part of boundary modelled to be be connection point.

  • Slit: 4" or 6"
  • Exposure time: 30 s
  • X positions: 224 (4") / 160 (6")
  • FoV: 16' x 11'
  • Observation time: 1.9 / 1.3 hours per study
  • Nº repeats: depends on target


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

  • At perihelion 6 rasters. Full north-south raster only to be done for extended holes. Otherwise it is enough to point at the boundaries, it could be that only one raster is enough.

  • For stable structures: 3-4 days of standard observations + 1 day of mosaic.

  • Highest possible resolution is preferred.


Lines for SPICE Composition Mapping:

– 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,

  • 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

Lines for SPICE Dynamics:
– 4 profiles + 6 (2?) intensities:
  • 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) 


Estimate for daily mosaic with 4 pointing positions of full rasters (6" slit, 10s exptime, few strong lines, 30mins duration): 10 x 4 x 9.84Mb = 0.4Gbits (18% of orbital vol)

EUI

FSI Synoptic mode (S) (FSI174)

Cadence of a few hours around s/c magnetic connection point

Synoptic observations with FSI174 (perhaps partial frame)
PHI

Regularly spaced FDT images for I_cont, B_LOS, gamma and phi.

Cadence of 6 hours

PHI_synoptic_FDT_4 (with 6hrs cadence)

Throughout RSW.

Metis

Global maps of v_outflow in corona

Global n_e maps

Brightness fluctuation spectra

  • WIND ≥ 2 hr, at 5 min cadence
  • MAGTOP ≥ 2 hrs, twice a day, at 5 min cadence, during perihelion RSW
  • FLUCTS ≥ 1 hr, at 10s cadence, VL intensity only


SoloHIMeasure solar wind speed above potential source region in co-ordination with Metis
STIXN/A


Science objectives


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

Operational constraints 

Additional comments
1.1.2.1 Does slow wind originate from the over-expanded edges of coronal holes?Coronal hole(s), Coronal hole boundary.

few hours per day

  • South RSW
    • High latitude observing is ideal for polar coronal holes.
  • Perihelion RSW

    • good if coronal hole has equatorial extension.

  • Earth view beneficial before RS window for magnetograms to estimate global solar magnetic field
SPICE mosaic for mapping.

Best if s/c is on same streamline as SPP, but not required



1.1.2.2 Does slow and intermediate solar wind originate from coronal loops outside of coronal holes?




1.1.2.3 Abundance of minor ions as a function of height in the corona as indicator of slow or fast wind



(this objective should be expanded, including also the abundance of minor
  ions as a function of latitude, particularly across the coronal hole/streamer boundary)

Instances run / planned

LTP6:

2022-03-22 to 30 (SOOP Coordinator: D. Spadaro)

LTP9:

2022-10-27 (SOOP Coordinator: D. Spadaro)

LTP11:

2023-04-09  (SOOP Coordinator: D. Spadaro)

Science outcomes

Ref of paper using the SOOP data

Original SOOP proposers

D. Spadaro, E. Antonucci, A. Giunta, C. Owen

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1 Comment

  1. Anik De Groof

    SOOP ID in SOOP Kitchen = LB1