Proposed SOOP Coordinators
T. Horbury
Description
Standard In situ operations out of remote sensing windows. Will contribute to all in situ only objectives. Coordinated bursts schedules to obtain equal coverage in heliocentric distance rather than time.
Instrument | Mode | Comment |
EPD | Normal + Burst |
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MAG | Normal + Burst |
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RPW | Normal + Burst | Triggers Active |
SWA | Normal + Burst |
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SAP objective | Target | Duration | Opportunity(e.g., orbital requirements, solar cycle phase, quadrature ...) | Operational constraints | Additional comments |
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2.3.2.2 Identify interplanetary shocks and characterise their spatial and temporal evolution | In Situ | Sufficient Coverage for good statistics | Multi spacecraftstudy(SPP) in multiple orientations (radial, spiral, quadrature alignments) – should come for free. | EMC Quiet | Burst modes scheduled for flat radial coverage |
In Situ | Sufficient Coverage for good statistics |
| EMC Quiet | Burst Modes,mostlytriggered. | |
In Situ Heliosphere | Sufficient Coverage for good statistics | Radial dependence | EMC Quiet | Normal + Burst modes Triggered by RPW (this is important to know for low telemetry periods when the triggering would be de-activated).
SPP Good to have. | |
2.3.5 Understand the radio emissions from the ICME driven shocks | In SItu | Sufficient Coverage for good statistics | Good coverage of different radii | EMC Quiet | RPW Triggers important. |
In Situ | Sufficient Coverage for good statistics | Good coverage of different radii and latitudes | EMC Quiet | Normal Mode Sufficient | |
1.1.2.6 Disentangle the spatial and temporal variability of the slow wind | In Situ |
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1.1.2.8 Determine the velocity, acceleration profile and the mass of the transient slow wind flows | In Situ |
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In Situ |
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1.2.2.1 Determine where energy is deposited in the solar wind |
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1.2.2.2 What drives the evolution of the solar wind distribution functions in situ? |
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| EMC Quiet |
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In Situ Seed population specification from the heavy ion composition of solar wind and suprathermals in the inner heliosphere timing | Statistics
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| Normal mode sufficient. | |
3.1.1.3 How are superhalo particles accelerated continuously in the corona and solar wind?
| In Situ Particles acceleration | Statistics | Good radial spread. | However, SPICE could be used to observe non-thermal electron distributions at the limb, e.g in combination with SPP in quadrature. However, if SPICE cannot observe the superhalo energies, then it is not needed here (TBC). | |
| 3.1.1.5 Do proton-amplified Alfvén waves play a role in accelerating particles at shocks? | In Situ Alfvén waves role in SEP acceleration | Statistics
| Perihelion | SWA Burst mode | |
In Situ | Statistics
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| EPD (SIS) Normal mode sufficient SWA/MAG/RPW not needed RS window not necessarily needed (for this specific objective), however it would be great if we can identify the solar source as for all Objective 3 (SPICE would be nice to have) It seems to be feasible with SIS. | |
In Situ | Statistics
| Perihelion |
| Normal + Burst modes | |
| 3.2.4 How do large and small-scale structures modulate particle fluxes? | In Situ Corona + Heliosphere | Long term observations | Radial dependence RS context is good to have (not necessary). | Good to have Metis compatible | May need full-disk RS + Metis for context. SWA regular scheduled and triggered burst by RPW (Multiple bursts per day only needed for the small-scale structures but we cannot predict when this will happen in order to plan for multiple scheduled bursts per day, except if we know we are in a particularly active period. Large scale CIRs/ICMEs may rather need triggered burst) |
| 3.2.0 What controls the escape of the particles to the heliosphere? | In Situ Heliosphere | Statistics | Perihelion | EPD MAG RPW | |
| 1.1.3.2.3 How does the heliospheric magnetic field disconnect from the Sun? | In Situ Heliosphere | Radial dependence & Perihelion | |||
| 3.2.1.2 Measurements of SEP events time profiles and anisotropy in order to probe solar wind turbulence | In Situ Heliosphere | Statistics | Close to perihelion and different range of distances | Needs to be done for a range of distances to monitor the SEP contributions from solar source and IP turbulence. Also partly addressed by L_IS_STIX and better by L_IS_SoloHI_STIX. | |
| 3.2.1.3 Identify dropouts and measure scattering of SEPs by turbulence. |
1 Comment
Anik De Groof
SOOP ID in SOOP Kitchen = IDF