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General description

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

Triggers: disabled

Observations requirement (baseline)

EUIEUV & LYA Coronal hole modes (C) 600 s cadenceEUV + Lyman alpha, FOV and resolution matching PHI


SPICE Dynamics (bracketed by SPICE Composition Mapping)2" slit, 128 slit positions, scan duration 11 minutes
PHIPHI_magnetograph_FDT/HRT_2 HRTFull FOV, 10 min cadence, 5 quantities, 2x2 binning
MetisMETIS standard modes: MAGTOP or GLOBALMetis can potentially provide context data before and after the 15 day SOOP (offpointing during the 15 days)

Science objectives

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

Operational constraints 

Additional comments AR , complex AR on E limb15 daysPerihelion: to ensure near-co-rotation,
Stereoscopy, which constrains Earth-Sun-SC angle
Duration 15 daysPotentially coordinated with  ground based DKIST/EST/GREGOR/NST for short-term studies What is the distribution of the open magnetic flux?

coronal holes, QS, AR Contribution of flare-like events on all scales

increase cadence; only partially Detect and characterise waves in closed and open structuresplumes

high latitude pointing Magnetic reconnection in the chromosphere, the transition region and the corona

increase cadence
( CME initiation) probably better FDT Track granules and magnetic features to follow their motion and interactions

increase cadence Follow individual magnetic features flux from lower to high latitudes 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)

Science outcomes

Ref of paper using the SOOP data

Original SOOP proposers

Luis Bellot-Rubio, Andrzej Fludra, S. Parenti

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1 Comment

  1. SOOP ID in SOOP Kitchen = RS0