No request, but if spectral data is available for coronal hole observations, we can measure temperature, density and flow speeds and we might expand our photospheric studies to studies at upper layers, such as the source of solar winds and connectivity to the heliosphere.
Study 000582: ACRONYM: HOP81_new_study This is the same study that is used for HOP 81. It performs a large scan of the polar region in coordination with SOT/SP measurements of the magnetic field. TARGET : Coronal hole EXPOSURE TIME : 50s RASTER : Scanning SLIT : 2" (was 1") STEP_SIZE : 4" (was 1") FOV : 322"x384" SPECTRAL WIND.: 24 (was 12) DATA COMP. : DCPM RASTER DURATON: 1h14m DATA VOLUME : 140 Mbits (was 150 Mbits) LINES : Fe VIII, Fe X, Fe XI, Fe XII, Fe XIII, He II, O V, Mg VI, Mg VII, Si VII, Si X Fe IX, Fe XIV, Fe XV, Fe XVI, S X, Ar XI POINTING: -------- Polar coronal hole with fixed pointing. Make sure to cover SOT FOV and the solar limb.
INSTRUCTION TO PLANNERS: ----------------------- Start this study at the beginning of the SAA free period (roughly 10-15UT). Repeat the study several times avoiding Hinode eclipses. The later part may coincide with a short SAA. Note: The plan for FSM is the same as that for DSM.
WARNING: ------- Avoid SAAs as much as possible (SAA degrades data compression factors and mutilates the data) |
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