Joint Planning of SOT/XRT/EIS Observations Outline of 90 Day Initial Observing Plans

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

2. SOT Initial Science Plan Principal Topics • 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

3. XRT Initial Science Plan Principal Topics • Flares fromdynamic 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

4. EIS Initial Science Plan Principal Topics • 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, Te and ne 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, ne 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, Te and ne in surrounding regions -Register and follow eruption

5. 90 Day Observing Programme Summary

6. 90 Day Observing Programme Summary

7. Coordination with Other Missions • Coordination with STEREO imaging should occur in first • 90 days • Coordination with TRACE and SOHO/ MDI also necessary Actions • 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)

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9. 4. Initial Science Plan Background • 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

10. 4. Initial Science Plan Line Lists • 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

11. 4. Initial Science Plan Principal Topics • Flare trigger and dynamics: - Spatial determination of evaporation and turbulence in a flare • Active region heating: - Spatial determination of v, Te and ne 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

12. 4. Initial Science Plan Flare Trigger and Dynamics • 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)

13. 4. Initial Science Plan Active Region Heating: • Spatial determination of v and ne in AR loops for range of Te 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

14. 4. Initial Science Plan Quiet Sun Studies: • Correlate coronal Te, ne 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 andSi 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