L_SMALL_HRES_HCAD_Slow-Wind-Connection

General description

Science Goal: What are the release mechanisms of the slow solar wind at an open-closed magnetic field boundary? (See Slow Wind SOOP slides)

Aims:

Link in-situ plasma to specific coronal source regions,
Observe the magnetic field configuration and its evolution at open-closed boundaries
Identify possibly signatures of interchange reconnection at open-closed boundaries

Target: active region/coronal hole boundary, dependent upon magnetic connectivity

Default SOOP duration: 3 days

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

Triggers: only IS triggers enabled

Observations requirement (baseline)

Instrument	Mode	Comment
EPD	EPD_NEW_CLOSE_BURST	close mode + scheduled/triggered burst
MAG	MAG_EQUAL8_BURST	normal + scheduled/triggered burst Low-latency data useful
RPW	RPW_NORMAL_HIGH1	normal + scheduled/triggered burst
SWA	SWA_PAS_NORMAL11_BURST_11	normal + scheduled/triggered burst Low-latency data useful
SPICE	Combination of: SPICE_SPECTRATLAS, SPICE_COMPOSITION, SPICE_DYNAMICS	Raster area should be optimised to make sure open-closed field boundary is captured Line choices optimized for type of target Run combination of: - spectral atlas, full spectrum, FOV=2’x11’, duration ~53 minutes - A composition map, 60 s exposure time, FOV=10.6’x11’, duration of 2.7 hours, lines included: O III 70.3 nm multiplet Mg IX 70.6 nm 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 C III 97.7 nm O VI 103.2 nm - slow dynamic study (synoptic type), 30 s exposure time, FOV=12.8’x11’, duration of 1.6 hours, 5/6 repetitions of this study according to the time available and spacecraft constraints (e.g. WOLs, HGA_PT), spectral lines included: O III 70.3 nm multiplet Mg IX 70.6 nm O II 71.8 O V 76.0 nm multiplet N IV 76.5 nm Ne VIII 77.0 nm S V 78.6 nm O IV 78.7 nm C III 97.7 nm H I 1025 nm O VI 1032 nm
EUI	EUV & LYA Coronal hole modes (C) (uses HRI) at 6s cadence FSI Synoptic mode (S) throughout at 900s	If TM is limited, varying priority schema can be used to keep HRI data manageable (FSI_Synoptic_B)
PHI	Regularly spaced HRT data at medium to high resolution (~3-5 mins) e.g. PHI_raw_HRT_6 + regular PHI_synoptic_4	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
Metis	METIS_GENERIC	for context and linkage of solar wind source regions to SC Only applicable if beyond ~0.5AU during target tracking
SoloHI	HI_SYN_MID	Context via SoloHI synoptic modes
STIX	STIX_BASIC STIX_ANALYSIS	not strictly needed for SOOP although context is appreciated

Science objectives

SAP objective	Target	Duration	Opportunity/Orbital configuration	Operational constraints	Additional comments
1.1.2.2 Does slow and intermediate solar wind originate from coronal loops outside of coronal holes?	coronal loops outside of coronal holes	few 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
1.2.2.6 Study fast plasma flows from the edges of solar active regions discovered with Hinode/EIS	edges of solar active regions - at most likely ballistic connection point	few 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
1.1.4.1.1 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
1.2.2.5 Magnetic reconnection in the chromosphere, the transition region and the corona
	Quiet Sun at various latitudes.	several days	low + 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

Instances run / planned

LTP6 (run):

2022-03-03 to 06, 2022-03-17 to 22 (SOOP Coordinators: S. Yardley)

The slow wind connection SOOP operated with the baseline observations outlined above.

LTP11 (planned)

2022-03-30 to 04-02, then 2023-04-22 to 04-24 (SOOP Coordinators: S. Yardley, A. James)

Science outcomes

Yardley et al. (2022, in prep): Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage

Ngampoopun et al. (2022, in prep): Southern Polar Coronal Hole Boundary: Investigating the eruption of a filament channel and its merging with the southern polar coronal hole

Boundary

Baker et al. (2022, in prep): Observational Evidence of S-web Source of Slow Solar Qind

Berghmans et al. (2022, in prep): First Perihelion of EUI

Further information

(see Yardley et al. 2022, in prep)

RSW1 Target: NOAA active region complex including ARs 12955, 12957, 12961

RSW2 Targets:

Southern polar coronal hole boundary (2022-03-17 06 UT – 2022-03-18 18:40 UT)
NOAA AR 12967 (2022-03-18 18:40UT – 2022-03-22 00UT)

Coordinated Observations: Hinode and IRIS through IHOPs 433 and 434.

Original SOOP proposers

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

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