In the interval October 2 to October 15 2024: - The first map should taken at 09:00 UT. This will coincide with the EUI/HRI high-resolution and high-cadence burst (from 09:00 to 10:00 UT on Oct 2-5 and Oct 12-15 and 09:15 to 09:45 UT on Oct 6,7,9,10,11) and the suitable time for the SST and GREGOR coordination. - The second map should be taken at 19:00 UT. This will coincide with the second EUI/HRI high-resolution and high-cadence burst (19:00-20:00 UT on Oct 8 and 19:15-19:45 UT on Oct 6,7,9,10,11), and the suitable the DKIST coordination. - On October 8, there will be a Solar Orbiter interruption from 00 UT to 14 UT. However the SST and GREGOR team will keep following the same target if the seeing conditions are suitable. We leave it at your discretion to decide whether you wish to keep the first map on this day.
If the telemery allows it, SOT observations could follow the previous request of HOP 0442. Priority on times when PHI/HRT observes (see the "time window" section) and more specifically during coordination time with DKIST and SST&GREGOR, that will happen at late and early UT hours, respectively.
Since Solar Orbiter can, to some approximation, co-rotate with active regions (ARs), it allows a longer follow-up, thus allowing to investigate how much can TNE cycles last. Observations are currently limited to the follow-up of active regions during their passage on-disk, and the length of TNE cycles is constrained by this artificial limitation (6.5 days with limited distortion). The AR long-term evolution SOOP will take place between 2-16 October 2024, and it aims at capturing from the unique standpoint and capabilities the major aspects of TNE cycles in the solar corona and will try to address two main scientific questions: Q1: How long do they last? How/when do they start and stop? Q2: Are these cycles producing elemental abundances variations? We will be interested in long-period EUV pulsations (with the continuous 10-min cadence EUI/FSI observations). These pulsations reflect the density and temperature changes for coronal loops undergoing TNE. We will also aim to observe coronal rain during the cooling phases of these cycles (EUI/HRI observations, 5 s cadence for one hour every day). PHI/HRT will also run at a cadence of 60-min at hh:30 (so it always falls mid-time of the HRI windows). With SPICE (64-min rasters: 64 slits positions, 60-s exposure and 6" slits).we will explore for the first time whether these cycles produce characteristic elemental abundance variations. These cycles involve chromospheric evaporation and abundances are set in the chromosphere. In order to get these continuous composition rasters, we will thus not look at the dynamics with SPICE.
We would thus like to complement these observations with in particular EIS observations, to focus on the coronal flows related to TNE. |
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