Decay of Active regions: see slides in 4-Bellot-Rubio-SAP4_magnetoconvection5_final.pptx:
Decay process of ARs is not well known:
- Slow, may last a few weeks
- ARs approach limb and suffer from projection effects
- Emerging flux starts to reconnect with preexisting flux very soon
- Appearance of filaments, flux rope eruptions and CMEs in late phases of decay
- Sunspot fragmentation by light bridges?
- Flux erosion by convective flows?
- Role of moving magnetic features?
- How is the AR flux dispersed?
- What is the fate of the flux?
Default SOOP duration: 15 days
Pointing requirements: target pointing and tracking
Observations requirement (baseline)
|EUI||EUV & LYA Coronal hole modes (C) 600 s cadence||EUV + Lyman alpha, FOV and resolution matching PHI|
|SPICE Dynamics (bracketed by SPICE Composition Mapping)||2" slit, 128 slit positions, scan duration 11 minutes|
|PHI||PHI_magnetograph_FDT/HRT_2 HRT||Full FOV, 10 min cadence, 5 quantities, 2x2 binning|
|Metis||METIS standard modes: MAGTOP or GLOBAL||Metis can potentially provide context data before and after the 15 day SOOP (offpointing during the 15 days)|
(e.g., orbital requirements, solar cycle phase, quadrature ...)
|188.8.131.52||Isolated AR , complex AR on E limb||15 days||Perihelion: to ensure near-co-rotation, |
Stereoscopy, which constrains Earth-Sun-SC angle
|Duration 15 days||Potentially coordinated with ground based DKIST/EST/GREGOR/NST for short-term studies|
184.108.40.206 What is the distribution of the open magnetic flux?
|coronal holes, QS, AR|
|220.127.116.11 Contribution of flare-like events on all scales||increase cadence; only partially|
|18.104.22.168 Detect and characterise waves in closed and open structures||plumes|
high latitude pointing
|22.214.171.124 Magnetic reconnection in the chromosphere, the transition region and the corona||increase cadence|
|(126.96.36.199 CME initiation) probably better FDT|
|188.8.131.52 Track granules and magnetic features to follow their motion and interactions||increase cadence|
|184.108.40.206 Follow individual magnetic features flux from lower to high latitudes|
|220.127.116.11 How supergranular flows facilitate/impede transport of magnetic features?||increase cadence|
Instances run / planned
2022-03-31 to 04-04 (SOOP coordinators: L. Bellot )
2022-10-16 to 27, 2022-10-29, 2022-11-01 to 06 (SOOP coordinators: S. Parenti, G. Valori)
Ref of paper using the SOOP data
Original SOOP proposers
Luis Bellot-Rubio, Andrzej Fludra, S. Parenti
Anik De Groof
SOOP ID in SOOP Kitchen = RS0