Plots are in GSE (geocentric solar ecliptic) coordinates, so Earth is at [0,0], the Sun is at [1,0]. The plot is the projection of the orbit on the ecliptic plane.
6th orbit + first part of 7th orbit in EMP: 4 RS windows, N and both S windows reach max latitude 31º ; perihelium at 0.3AU.
RS window (default) placement
Safe Mode Comms Blackout
- IF PERIHELION WINDOW GETS SHIFTED FEW DAYS EARLIER (also good for TM):
connection science goals on slow solar wind sources. These require modelling to find the most likely connection point.
SOOPs L_SMALL_MRES_MCAD_Connection_Mosaic combined with L_SMALL_HRES_HCAD_SlowWindConnection (higher res/cadence RS to explore source region in more detail) or L_SMALL_MRES_MCAD_Ballistic-connection
If we happen to point at a coronal hole boundary, also the SOOP L_SMALL_HRES_LCAD_CH_Boundary_Expansion fits.
- close perihelion also candidate for R_SMALL_HRES_LCAD_Fine-Scale-Structure
MTP17 - full orbit (first 3 windows):
- RS observations can run from pole to pole with minimal interruption. This is particularly interesting for L_BOTH_LRES_MCAD_Pole-to-Pole SOOP.
- Alternatively, or in combination, run L_SMALL_HRES_HCAD_Fast-Wind to address science goal 184.108.40.206 Low FIP fast wind origins: fast scan through big range of latitudes, and low-latitude coronal hole would be ideal
- Other candidate: run R_FULL_HRES_HCAD_Density-Fluctuations at each RSwindow (not too far out for Metis to still see the density fluctuations). 8 hour per window should be enough.
MTP17-North = close high-lat window
- same SOOP as above L_SMALL_HRES_HCAD_Fast-Wind can be used to address science goal 220.127.116.11 Origin of the small-scale X-ray and UV jets in polar coronal holes