This covers half of SOOP 2.1 from the MPS Document, the other half is covered by L_SMALL_HRES_HCAD_Slow-Wind-Connection
Default SOOP duration: Several days
Pointing requirements: Quiet Sun
Pradeep Chitta (Proposed)
The emergence, diffusion and decay of ephemeral regions near the poles and below high- latitude coronal holes should be studied for the aspect of how they feed the magnetic network (see e.g. Simon et al. 2001, ApJ 561, 49 427; Gosic et al. 2014, ApJ 797, ). In particular, the latitudinal dependence of this decay process would be interesting to study.
|PHI||PHI_nominal_HRT_0 but subfielded, 1-2 min cadence and no binning||Half FoV 1-2 minute cadence, 5 quantities, highest resolution|
|EUV & LYA Coronal hole modes (C)||FOV and cadence matching PHI, 15-30s cadence|
|SPICE||SPICE Composition Mapping||FOV Matching PHI|
(e.g., orbital requirements, solar cycle phase, quadrature ...)
|4.1.1 Study the detailed solar surface flow patterns in the polar regions, including coronal hole boundaries.||-||-||see Helioseismology SOOPs||-|
|4.4 Are there separate dynamo processes acting in the Sun? (188.8.131.52)||Ephemeral Regions, (quiet Sun below the poles, above polar coronal holes).||Several Days||High latitude, solar minimum||feature tracking|
This SOOP also covers the science proposal of Rafael Manso Sainz: "Broken Axial Symmetry of Global Magnetic Field":
It has been also shown that the poles of the dipole field are not aligned with the rotation axis (Livshits & Obridko 2006; Pastor Yabar et al. 2015). All these issues, related to the global axial symmetry, or lack thereof, could be most clearly settled by observations from the poles and/or simultaneous observations of the whole Sun (SO and Earth in opposition). From the synoptic global field maps one can also interpolate to the time when the dipole was best aligned and determine its minimum deviation from the pole during polarity flip between two solar cycles.
Two types of observations have to be carried out:
This SOOP covers also the scientific idea of Maarit Käpylä / Jörn Warnecke: "Helicity mapping for dynamo studies" (see TN by Johann Hirzberger, section 2.6, proposed SOOP#1. The proposed SOOP#2 comes for free with most of the synoptic type of SOOPs and the pole-to-pole one).
The magnetic and kinetic helicity plays an important role for the solar dynamo and its connection to heliosphere. Particularly important is to know how these helicities are distributed as a function of latitude. Low latitude measurements have already been done using space-based and ground-based telescopes, however, with the exception of Ulysses, the high latitudes have not been accessible. As Solar Orbiter in its extended mission phase will reach latitudes up to 33", it provides a unique opportunity to use the SO/PHI instrument to measure the kinetic and magnetic helicities at high latitudes and near the poles. Furthermore, with the in-situ magnetic field measurements, we have the possibility to determine the helicity distribution as function of latitude and its transport from the photosphere to the heliosphere.
Anik De Groof
SOOP ID in SOOP Kitchen = RS2