Proposed SOOP Coordinators
D. Spadaro, A. Vourlidas, D. Williams
Description
Synoptic SOOP designed for CME science and global coronal structure. Typically runs for a whole RS window.
Default SOOP duration: 10 days
Pointing requirements: disk centre
Triggers: IS + Metis triggers active
| Instrument | Mode | Comment |
|---|---|---|
| EUI | FSI Synoptic mode (S) | 10 min cadence |
Metis | METIS standard modes: GLOBAL mode, METIS special modes CMEOBS whenever triggered (model as max 3 CMEs per RSW) | CME Watch On |
| PHI | FDT Synoptics: PHI_synoptic_FDT_4 with 6hr cadence | 6 hour cadence |
| SoloHI | Normal Operations: SYN + SHOCK (at perihelion) (modelled as HI_SYN_NEAR for now) | |
| SPICE | N/A | |
| STIX | STIX Normal Mode | |
| EPD | Normal + Burst Mode | |
| MAG | Normal + Burst Mode | |
| RPW | Detection Mode | Burst Triggers Active |
| SWA | Normal + Burst Mode |
| SAP objective | Target | Duration | Opportunity (e.g., orbital requirements, solar cycle phase, quadrature ...) | Operational constraints | Additional comments |
|---|---|---|---|---|---|
| 2.1.1.2 CME structure | Full Disk | Long Duration | Quadrature ideal, perihelion would be best, but useful at all distances. | No Offpoints | For EUI could do onboard prioritisation to increase cadence - discard 9/10 images unless there's a trigger. |
| 2.1.1.3 CME evolution | Full Disk | Long Duration | Higher latitude orbits particularly interesting. Angular Separation from other spacecraft is a bonus | No Offpoints | Temperature evolution from Metis in UV |
| 2.2.1 How do CMEs contribute to the global evolution of magnetic flux in the heliosphere? | |||||
| 1.1.3.2 How does the Sun's magnetic field link into space? | Corona + Heliosphere | Metis compatible | Coordination with SPP is a bonus | ||
| 1.1.3.3 What is the distribution of the open magnetic flux? | |||||
| 1.3.3 Plasma turbulence variability | Full Disk | Long Duration | Perihelion good for SoloHI contribution Several Latitudes | No Offpoints EMC Quiet | Radial alignment with SPP useful |
| 1.3.4 Plasma turbulence anisotropy | Full Disk | Long Duration | Radial Dependence, | EMC Quiet No Offpoints | SPP important to have |
| 1.2.1.10 Heating in flaring loops vs heating in active regions | Full Disk | Long Duration | More statistical study: having STIX on, observing all the flares and using EUI synoptics to find out about the source region | N/A | |
| 3.1.2.2 Evaluate how significantly large flares contribute directly to gradual SEP events | Corona & Heliosphere | Statistics | Near perihelion in order to get 'as-pure-as -possible' signal | Metis compatible | FSI 10 min cadence (default) SoloHI, Metis, STIX Low resolution does not seem to be a problem |
3.1.4.1 Hard X-ray emission of escaping electron beams (thin-target emission) | Corona | Statistics | Near perihelion to get best spatial resolution with STIX | RPW STIX | |
3.1.4.2 X-ray emission from electrons accelerated at CME shocks | Corona & Heliosphere | Statistics | NOT at Perihelion | Metis compatible | RPW STIX Metis We cannot hunt for this event (too specific requirements: CME lifting off from behind the limb to shield the X-rays from AR footpoints, to allow STIX to observe hard X-rays from shock) and we hope we get it for free through this SOOP |
4.2 What are the properties of the magnetic field at high solar latitudes? [source: SOL-PHI-MPS-MN5100-TN-2] | Full disk | synoptic during solar minimum | opposition with NEO | Co-observations with NEO global field maps |
2 Comments
Andrew Walsh
3.1.7.2 goes here, not at perihelion
Anik De Groof
SOOP ID in SOOP Kitchen = LF5