1.2.1.7 Detect Detect and characterise waves in closed and open structures (e.g. De Pontieu et al., 2007), looking for signatures of their dissipation in the transition region and low corona, with a corresponding evaluation of the energy released to heat the solar plasma.
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Targets: AR (also closed loops in QS?), on-disk and also off-limb (for spicules).
Spicules:
Maybe divide this objective per target?
Operational requirements table:
Requirement | YES / NO / Not required / MAYBE / GOOD TO HAVE / NUMBERS | Remarks |
|---|---|---|
| Duration of the observations | ? | |
| Perihelion | Good to have | |
| RS window | Yes | |
| High latitude | Not required | |
| Solar cycle dependence | Good to have | |
| Radial dependence | No | |
| Linkage science | No | |
| Multiple orbits | Good to have | |
| Far side observations | No | |
| Earth observations | Good to have | |
| EMC Quiet | No | |
| SPP | No | |
| Instruments | EUI, PHI, METIS | RS only |
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PHI,
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HRT medium resolution data
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Requirement
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FOV [pixels]
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1024 x 1024
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Parameters
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Ic, vLOS, B, γ, φ (interlaced with raw data)
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duration
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2 days
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cadence
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1/(1 min)
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N orbits
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2
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solar distance
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entire orbit
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PHI operating mode
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3+8
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co-ordination
?
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- Measurement of the solar wind outflow velocity gradient in the outer corona, to localise regions of energy deposition, via Doppler dimming of the HI Lyα intensity in the field of view 1.5-2.9 degrees. Measurement of the magnetic field topology through the global corona configuration. Measurements of the brightness fluctuation spectra.
- Products:
- Global maps of outflow velocity in corona.
- Global maps of the electron density in corona/coronal configuration.
- Brightness fluctuation spectra.
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- WIND (min. obs time 2 hr, data volume ≤ 300 Mb)
- MAGTOP (min. obs time 2 hr, data volume ≤ 480 Mb)
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- FLUCTS (min. obs time 1 hr, data volume ~ 2 Gb) at perihelion.
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