General description

This SOOP is designed to study the dynamics and fine structure of magnetic features in the atmosphere using all RS instruments except Metis and SoloHI. The observations are performed during several hours at the highest spatial resolution with high (but not maximum) cadence.

This SOOP can be used on different targets, from active regions to quiet Sun to coronal holes to polar regions. 

Specific questions for active region targets:

  • Flows in and around sunspots
  • Sunspot oscillations
  • Moving magnetic features
  • Flux cancellation at boundary of sunspot moat and effects in higher atmospheric layers
  • Magnetic/velocity stereoscopy of sunspot features



  • Target a region visible from Solar Orbiter and Earth simultaneously
  • Perform high-res, high-cadence observations for several hours
  • Monitor different atmospheric layers
  • Coordinate with Earth-bound assets (for stereoscopy)


Default SOOP duration: 4 hours (minimum: 1 hour). Can be run for up to 6-8 hours

Offpointing requirements: Quiet Sun targets will be observed at the disk center and different heliocentric angles. Active region and coronal hole targets will be observed outside of the disk center.

Triggers: disabled


Observations requirement (baseline)



PHI_nominal_HRT_0 (HRT)

1 min cadence. Minimum FOV of 1024 x 1024 pixels (full FOV if TM allows).

no binning.

FSI Synoptic mode (S) and, depending on target,

EUV & LYA Quiet Sun modes (Q) or EUV & LYA Coronal hole modes (C)

FSI174 and FSI304 observations at 10 min cadence during entire SOOP duration

plus 1-hour HRI bursts with following parameters: 

  • HRIEUV: 10 s cadence (faster if TM allows)
  • HRILYA: 30 s cadence

Rapid dynamics rasters with 15 min cadence or faster, over similar FOV as PHI and EUI/HRI.

Example: Study ID 2123

4" slit, step size=4", row_height=768, exposure= 5s, n_exposures=160, n_profiles=8
STIXSTIX Normal Mode

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

Operational constraints 

Additional comments Full characterization of photospheric magnetic fields and fine structures

Quiet Sun

Coronal Holes

1 h per target

Perihelion for quiet Sun

High-latitude window for coronal holes

Reduced FoV (1024x1024 for PHI, equivalent for others) Photospheric reconnection

Quiet Sun

Coronal Hole

Active regions

2 hours per target

Perihelion for quiet Sun and sunspots

High-latitude window for coronal holes

Full FOV.

Composition mode may be useful for SPICE too.

4.2.2 Basic properties of solar high-latitude magnetic field structuresPolar regions1 h per targetHigh-latitude window for coronal holes

Reduced FOV (1024x1024 for PHI, equivalent for others)

4.3 What is the nature of magnetoconvection?

4.3.5  How do magnetic fields emerge on the solar surface

Quiet Sun

(disk center, E/W limb, N/S polar region)
3 h per pointing (to secure good statistics)

Perihelion for highest resolution

Reduced FOV (1024x1024 for PHI, equivalent for others).

Coordination with space-borne assets (Hinode, IRIS)

5.5 Additional Science Objectives of PHI (Study flux appearance modes and interactions in QS)
[source: 4-Bellot-Rubio-SAP4_magnetoconvection5_final.pptx]

Quiet Sun (disk center, E/W limb, N/S polar region)3 hours per pointing (to secure good statistics)

Perihelion for highest resolution

First orbit & later in mission for higher latitudes

Reduced FOV (1024x1024 for PHI, equivalent for others).

Coordination with space-borne assets (Hinode, IRIS)

5.5 Additional Science Objectives of PHI What are the velocity and magnetic vectors in the solar photosphere?

[source: SOL-PHI-MPS-MN5100-TN-2, proposed by Alex Feller]

Disk centre (DKIST/FSP looking at solar limb)2 hoursPerihelion + quadrature with Earth

co-observations with DKIST/FSP, pointing at limb

Quadrature with Earth

Coordination with DKIST: FSP instrument pointing at limb 


5.5 Additional Science Objectives of PHI Interaction of oscillation modes and convection (stereoscopic helioseismology)

4.3.4  Magnetic oscillations in sunspots and active regions

Quiet Sun

Active regions

6 hoursPerihelion preferred,  r<0.5 au acceptablecoobs with near-Earth instrumentat ~30o

FOV as large as possible

Near-Earth instruments assumed to be continuously observing (HMI, GONG,...). If not, coordination will be needed.

Instances run / planned


2022-10-29 T02:00:00 to T06:40:00  (SOOP coordinator: Luis Bellot)

  • Successfully run for 4h40m
  • Target: AR 12131
  • Coordinated observations performed with Hinode/SOT/EIS and IRIS (HOP 447)


2022-11-04 T12:00:00->T23:59:00  (SOOP coordinator: Luis Bellot)

  • Planned to run for 6hours
  • Not run due to s/c anomaly


SOOP coordinators

Johann Hirzberger, Alex Feller, Luis Bellot Rubio, Andreas Lagg, Markus Roth, Susanna Parenti

  • No labels


  1. Modify to include composition and dynamics for SPICE and add objectives from Luis' presentation (SOOP2).

  2. Andreas' PHI PDF SOOP could also be included here.

  3. And also his Polar Features.

  4. Anonymous

    (Andreas Lagg):

    This SOOP contains also the scientific proposal of AlexFeller: "Limb stereoscopy of magnetic fields"

    FSP is designed to carry out highly sensitive Hanle diagnostics of solar limb magnetic structures. These measurements can be calibrated only if simultaneous high resolution photometric and Zeeman measurements are carried out from a much less inclined vantage point.

  5. PHI PI suggests to change the name to "Atmospheric" instead of "Photospheric". 

    Otherwise it makes no sense to have EUI and SPICE co-obs.

  6. SOOP ID in SOOP Kitchen = RS4