The European Space Agency
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
Strategy:
- 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)
|
Instrument |
Mode |
Comment |
|---|---|---|
|
PHI |
PHI_nominal_HRT_0 (HRT) |
1 min cadence. Minimum FOV of 1024 x 1024 pixels (full FOV if TM allows). no binning. |
|
EUI |
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:
|
|
SPICE |
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 |
|
|
STIX |
|
|
SAP objective |
Target |
Duration |
Opportunity |
Operational constraints |
Additional comments |
|---|---|---|---|---|---|
|
1.1.3.1 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) |
|
1.1.4.1.6 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 structures |
Polar regions |
1 h per target |
High-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 |
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 [source: SOL-PHI-MPS-MN5100-TN-2, proposed by Alex Feller] |
Disk centre (DKIST/FSP looking at solar limb) |
2 hours |
Perihelion + 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 5.5.3.1 Interaction of oscillation modes and convection (stereoscopic helioseismology) 4.3.4 Magnetic oscillations in sunspots and active regions |
Quiet Sun Active regions Sunspots |
6 hours |
Perihelion preferred, r<0.5 au acceptable |
coobs 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
LTP09
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
R_BOTH_HRES_HCAD_Atmospheric-Dynamics-Structure_LTP9.pdf
SOOP coordinators
Johann Hirzberger, Alex Feller, Luis Bellot Rubio, Andreas Lagg, Markus Roth, Susanna Parenti