R_SMALL_MRES_MCAD_Supergranulation

General description

Science Goal:

Supergranulation is an important convective scale that is distinguishable on the solar surface. Supergranules shape the magnetic network and thus play a role in the structuring of the upper solar atmosphere, including structuring of the solar wind. Properties of supergranulation (size and lifetime distributions, direct and indirect signatures in the upper solar atmosphere) closer to the solar poles are not well known.

Aims: Use Solar Orbiter polar observations to investigate the properties of convective and magnetic coupling through the solar atmosphere due to supergranulation near polar regions.

Target: polar regions

Default SOOP duration: 1-2 days

Pointing requirements: Target pointing and tracking

Triggers: disabled

Observations requirement (baseline)

Instrument	Mode	Comment
PHI	PHI_magnetograph_HRT_2	Partial FOV, 5 min cadence, 3 quantities (I_c, B_los, V_los)
EUI	EUV & LYA Coronal hole modes (C) -or- EUV & LYA Quiet Sun modes (Q)	HRIEUV FOV covering PHI FOV; 5–10 s cadence; 4´ 1–2 hours bursts covering the duration of PHI observations
SPICE	SPICE Dynamics	Matching the start of EUI burst sequences (preferred spectral lines: C II, C III, O IV, O VI, Ne VIII @ 770, Mg IX / Fe X). 2” slits and 128 steps. Exposure time of 10 s. 5–6 repeats per one EUI sequence

Science objectives

SAP objective	Target	Duration	Opportunity/Orbital configuration	Operational constraints	Additional comments
4.1.3 Explore the transport processes of magnetic flux from the activity belts towards the poles and the interaction of this flux with the already present polar magnetic field.	Supergranules	1-2 days	high latitude

solar orbiter