General description
This SOOP is aimed at observing structures in the outer corona and linking them to the heliosphere observed in-situ. Metis and SoloHI are leading this SOOP, while IS payload provides continuous observations. Synoptic support from other full disk RS instruments. Disk centre pointing preferred.
At high latitude:
This SOOP could be used as a whole- or half-orbit synoptic campaign that scans the Sun from one high latitude to the other (therefore mainly to be used later in the NMP at min inclination of 15º, i.e. orbit 3 or later). Close to the higher latitude windows, we get a radial sweep at nearly constant latitude for in-situ.
Default SOOP duration: 1 day
Pointing requirements: disk centre
Triggers: only IS triggers active
See SOOP 5 defined for SOWG8 planning exercise.
(SOOP will be modelled with 1 day duration, can be repeated as many times as needed)
Observations requirement (baseline)
| Instrument | Mode | Comment |
|---|---|---|
| SoloHI (leads) | SoloHI combination of high cadence TURB and synoptic mode (model as HI_SYN_NEAR for now) | disk center or stable pointing required |
| Metis (leads) | Generic program like WIND (METIS standard modes) interleaved with FLUCTS (METIS special modes) (FLUCTS runs 1 hr/day) At high latitude: One of METIS standard modes to observe large scale coronalstructures: GLOBAL or LT-CONFIG Model: LTCONFIG (cadence 20mins) and 3 x 1 hour CMEOBS | disk centre pointing preferred CME Watch On |
PHI | FDT synoptic: PHI_synoptic_FDT_4 | PHI may be processing in between observations. all data gets downloaded at higher latitudes, point to the poles for polar magnetic field observations. |
| EUI | FSI synoptic: FSI Synoptic mode (S) | all generated data gets downloaded |
| EPD | Normal Mode | |
| MAG | Normal Mode | |
| RPW | Detection Mode | Burst Triggers Active |
| SWA | Normal Mode | |
SPICE | SPICE currently proposes to use either SPICE Limb mode or SPICE Dynamics, depending on requirement for Metis-compatibility Limb target (not Metis-Compatible; SPICE Limb mode) :
Active region, if before or after Metis observatiosn (SPICE Dynamics) :
At high latitude: SPICE Composition Mapping raster followed by multiple instances of SPICE CME Watch |
Lines for SPICE Limb mode:
– 3 profiles and 3 intensities.
SPICE contribution is important for the measurements of line profiles, whose broadening can be considered a signature of the presence of waves in the atmosphere. SPICE observations near the limb can be carried out soon before and after those of Metis. SPICE scans many latitudes during the SOOP : large swath around the sun magnetic field spiral less curved at higher latitudes: Use observation called SPICE_CME_COMP in modelling. |
Science objectives
| SAP objective | Target | Duration | Opportunity (e.g., orbital requirements, solar cycle phase, quadrature ...) | Operational constraints | Additional comments |
|---|---|---|---|---|---|
| 1.1.2.7 Trace streamer blobs and other structures through the outer corona and the heliosphere. | Corona + Heliosphere | A few Days | Quadrature with Earth for combining SO RS with L1 IS and Earth Coronagraphs with SO IS | Metis compatible | Quadrature or radial alignment with SPP would be a bonus |
| 1.1.3.2 How does the Sun's magnetic field link into space? | |||||
| 1.3.2 How is turbulent energy dissipated and how does turbulence evolve within the heliosphere? | Corona + Heliosphere | Statistics | Radial Alignment with anything else. | Metis compatible | Radial alignment with SPP would be a bonus |
| 1.1.2.5 Structure and evolution of streamers | Corona + Heliosphere | Statistics | Quadrature with Earth for combining SO RS with L1 IS and Earth Coronagraphs with SO IS | Metis compatible | SPICE participates if possible. |
| 2.1.1.3 CME evolution | |||||
| 2.2.1 How do CMEs contribute to the global evolution of magnetic flux in the heliosphere? | |||||
| 2.2.2 What is the role of ICMEs in the Sun’s magnetic cycle? | |||||
| 2.3.1 Coronal shocks | Corona + Heliosphere | Statistics | Near perihelion for highest spatial resolution and best spatial coverage in the corona Earth side for radio obs from ground and magnetic field models for help with post facto analysis | Metis compatible | Quadrature with SPP would be a bonus |
| 2.3.2.1 Understand coronal conditions under which the shocks form and determine the interplanetary conditions where they evolve | Corona + Heliosphere | Statistics | Near perihelion for highest spatial resolution and best spatial coverage in the corona Earth side for radio obs from ground and magnetic field models for help with post facto analysis | Metis compatible | Quadrature with SPP would be a bonus |
| 2.3.2.3 Study heating and dissipation mechanisms at shocks with radial distance | Corona + Heliosphere | Statistics | Close to perihelion | Metis compatible EMC quiet | Burst modes most important here Metis needs to see within 5RS for Lyα |
| 2.3.2.4 Identify mechanisms that heat the thermal solar wind particle populations near shocks and determine their energy partition | Corona + Heliosphere | Statistics | Good alignment with SPP (Radial or Quadrature) would be beneficial | EMC quiet | Metis not strictly needed for this one but could still provide useful context. |
| 4.2 What are the properties of the magnetic field at high solar latitudes? |
Instances run / planned
LTP6:
2022-03-22 to 30 (SOOP coordinators: D. Spadaro + A. Vourlidas)
LTP9:
2022-10-08 to 12 (SOOP coordinators: D. Spadaro)
LTP11:
2023-04-06 to 09 (SOOP coordinators: D. Spadaro)
2023-04-20 (SOOP coordinators: D. Spadaro)
Science outcomes
Telloni D., et al., Observation of a magnetic switchback in the solar corona, ApJL, 936, L25, 2022
Original SOOP proposers
Vincenzo Andretta, Daniele Spadaro, Angelos Vourlidas
1 Comment
Anik De Groof
SOOP ID in SOOP Kitchen = LF1