1. Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans T. Shimizu, L Culhane

2. Solar-B SWG Meeting, ISAS, 21 st April, 2006 2 Active region tracking: - Emerging AR - Mature/decaying AR - Flaring AR - Subsurface flows - MHD waves Quiet Sun: - Network flux dynamics (Bright Points?) - Internetwork flux - Convective flow structure Irradiance: - Activity belt - Polar regions Prominences/Filaments - Prominence at limb/Filaments on disc - Track boundary evolution Local Helioseismology -Polar regions -AR tracking -Disc centre SOT Initial Science Plan Principal Topics

3. Solar-B SWG Meeting, ISAS, 21 st April, 2006 3 Flares from dynamic AR on disk:  Follow AR across disk, flare program loaded - Deploy range of filters and FoV sizes - Flare topology and energetics Track modest (emerging or decaying) active region on disc:  Image with large, medium and small FoVs - Structure, energetics and dynamic behaviour - AR evolution; track centre to limb? Quiet Sun/X-ray Bright Points:  Multi-filter study of bright points - Thermal structure - Dynamics - Life-cycle statistics Quiet Sun/coronal holes  Single filter for boundary imaging - Track boundary evolution Quiet Sun/filament  Magnetic structure around filament - Track filament for 1-2 days XRT Initial Science Plan Principal Topics

4. Solar-B SWG Meeting, ISAS, 21 st April, 2006 4 Flare trigger and dynamics:  Spatial determination of evaporation and turbulence in a flare - Characterize AR topology - Measure key structures in detail - Flare trigger response for early velocity measurement Active region heating:  Spatial determination of v, T e and n e in active region structures - High time cadence sit and stare observations; new dynamics - Observe AR global changes - Velocity measurements (± 3 km/s) Quiet Sun and coronal hole boundary:  Correlate coronal Te, n e and v with magnetic topology - Study corona above two supergranule cells - Study corona above bright point or explosive event - Observe above a coronal hole boundary Quiet Sun and Prominences (assume no available AR)  Spatial determination of v, T e and n e in surrounding regions -Register and follow eruption EIS Initial Science Plan Principal Topics

5. Solar-B SWG Meeting, ISAS, 21 st April, 2006 5 TopicSOTXRTEIS AR Tracking a) Emerging AR √√√ AR Tracking b) Complex AR/Flares √√√ AR Tracking c) Decaying AR √√√ Quiet Sun a) Network√Small events/ Bright Points Small events/ Bright Points Quiet Sun b) Intra- network √Small events/ Bright Points Small events/ Bright Points Spicules√Magnetic connections Prominences/Filaments√√√ 90 Day Observing Programme Summary

6. Solar-B SWG Meeting, ISAS, 21 st April, 2006 6 TopicSOTXRTEIS Helioseismology/AR Tracking √AR obs Helioseismology/QS/ Disc centre √QS obs Helioseismology/ Polar regions √Coronal HolesCoronal Holes/ Polar Plumes Irradiance/a) AR Tracking√AR obsAR obs/ irradiance? Irradiance/ b) Activity belt re-pointings √Small events Coronal Hole Boundaries√√√ 90 Day Observing Programme Summary

7. Solar-B SWG Meeting, ISAS, 21 st April, 2006 7 Coordination with STEREO imaging should occur in first 90 days Coordination with TRACE and SOHO/ MDI also necessary Coordination with Other Missions WIKKI to be established at ISAS or MSSL - as soon as practicable All three Solar-B instrument teams to post brief descriptions of their roles in above joint observing programmes (JOPs) Actions

8. Solar-B SWG Meeting, ISAS, 21 st April, 2006 8 END OF TALK

9. Solar-B SWG Meeting, ISAS, 21 st April, 2006 9 Aim of outline observing plan is to achieve critical science goals in the first three months after commissioning Goals identified but not yet prioritized: - Sun’s status in the period after launch will influence EIS and mission observing strategy on a weekly/daily basis Plan will need to be detailed and further enhanced 4. Initial Science Plan Background

10. Solar-B SWG Meeting, ISAS, 21 st April, 2006 10 Include three lines in ALL studies for a consistent dataset throughout the mission – core lines Core line list is: - He II → 256 Å, Fe XII → 195 Å, Ca XVII → 192.8 Å Selection based on line strength and temperature range Additional lines included as appropriate for each separate science objective Line Lists 4. Initial Science Plan

11. Solar-B SWG Meeting, ISAS, 21 st April, 2006 11 Flare trigger and dynamics: - Spatial determination of evaporation and turbulence in a flare Active region heating: - Spatial determination of v, T e and n e in active region structures Quiet Sun and coronal hole boundary: - Establish relationship between different types of quiet Sun event Boundary Conditions If solar conditions permit, observing time will be split evenly between topics An active region will be tracked if possible For AR with highly sheared magnetic field, EIS will be in flare mode to respond to XRT's trigger Otherwise observe quiet Sun and coronal holes for long periods (> 12 hrs) If no active regions but a quiet prominence, concentrate on this 4. Initial Science Plan Principal Topics

12. Solar-B SWG Meeting, ISAS, 21 st April, 2006 12 Spatial determination of evaporation and turbulence in a flare - Fast raster on pre-selected AR with a complex magnetic topology - Spectral imaging mode with 40” slot for a flare-productive AR - Flare trigger response from 250” slot to observe early velocity shifts - Line selection: core line list and Fe XXIV - 192 Å, Fe XV - 284 Å - FOV 200" X 200" with 2" slit - Cadence for 1 raster: 2.5 min with 1 s exposure - Windows to be wide enough for velocities of ~ 400 km/s (> 30 pixels) 4. Initial Science Plan Flare Trigger and Dynamics

13. Solar-B SWG Meeting, ISAS, 21 st April, 2006 13 Spatial determination of v and n e in AR loops for range of T e values  High time cadence sit and stare observations - - Spectral imaging with 40” slot/2s cadence to observe new dynamic phenomena - Alternate with 1” slit/2s cadence - Line selection: core lines and Fe XIII – 202 Å, - 203 Å  Spatial variation raster observations - Large raster (256” x 256”)/2” slit/20 sec cadence to observe AR global changes over several hours - Alternate with smaller raster (128” x 128”)/1” slit/40 sec cadence for detailed velocity measurements (± 3 km/s) - Line selection: core lines and Si VII – 275 Å, Mg VI – 269 Å, Fe X – 190 Å, Fe XI – 180 Å, Fe XIII – 202 Å, - 203 Å, Fe XIV – 274 Å, Fe XV – 284 Å, Fe XVI – 263 Å, Ca XIV - 193.8 Å, Si X – 258 Å  For suitable AR, follow from disc centre to limb comparing disc/limb structures 4. Initial Science Plan Active Region Heating:

14. Solar-B SWG Meeting, ISAS, 21 st April, 2006 14 4. Initial Science Plan Quiet Sun Studies: Correlate coronal T e, n e and v with magnetic topology inferred from SOT  Detailed study of corona above two supergranule cells; - Alternate 60” x 512” rasters with slot (40”) and slit (1”) - Spectral imaging (40” slot) for 50s cadence study of changes in morphology - Spectral imaging (1” slit) for high resolution 50s cadence spectra at fixed QS locations; insert 40” images for context - Line selection: core lines and Si VII – 275 Å, Mg VI – 269 Å, Fe X – 190 Å, Fe XI – 188 Å, Fe XIII – 202 Å, - 203 Å, Si X – 258 Å, - 261Å  Detailed study of corona above bright point or explosive event; - Raster, slot and field of view selections as above - Also run sit and stare mode - Line selection as above  Detailed study above a coronal hole boundary - Raster, slot and field of view selections as above - Also run sit and stare mode - Line selection as above