1. SOME COMMENTS ABOUT THE GIANT CHINESE SOLAR TELESCOPE CONCEPT JACQUES M. BECKERS Beijing August 6 – 8, 2011

2. OVERVIEW OF RECENTLY BUILD HIGHEST RESOLUTION SOLAR TELESCOPES

3. DUNN SOLAR TELESCOPE Sacramento Peak NM APERTURE76 cm VACUUM TELESCOPE (FIRST) ADAPTIVE OPTICS

4. SWEDISH SOLAR TELESCOPE La Palma, Canary Islands APERTURE100 cm VACUUM TELESCOPE ADAPTIVE OPTICS

5. DUTCH OPEN TELESCOPE (DOT) La PalmaCanary Islands APERTURE 50 cm OPEN AIR TELESCOPE

6. HINODE JAPANESE + TELESCOPE APERTURE50 cm SPACE FACILITY => No Seeing All Wavelengths

7. LARGEST AND BEST SOLAR TELESCOPE NOW: BIG BEAR NEW SOLAR TELESCOPE (NST) NST PARAMETERS Diameter1.6 meter Primary f-ratiof/2.4 λ Range.39 - 1.6 μm AOyes MCAO (DCAO)in future NST IS PROTOTYPE FOR ADVANCED TECHNOLOGY SOLAR TELESCOPE

8. COMPARISON OF HINODE WITH BBSO NST OBSERVATIONS DIAMETER = 0.5 DIAMETER = 1.6-m

9. LARGEST AND BEST CHINESE SOLAR TELESCOPE NOW: FUXIAN LAKE SOLAR TELESCOPE FUXIAN SOLAR TELESCOPE Diameter1.0 meter Primary f-ratio~ f/.92 λ Range0.32 - 2 μm AOin future

10. LARGE SOLAR TELESCOPES FOR THIS DECADE ADVANCED TECHNOLOGY SOLAR TELESCOPE (ATST) HALEAKALA, HAWAII APERTURE4-meter ADAPTIVE OPTICS (later MCAO) EUROPEAN SOLAR TELESCOPE (EST) LA PALMA or TENERIFE APERTURE4-meter MULTI CONJUGATE AO

11. ADVANCED TECHNOLOGY SOLAR TELESCOPE Completion 2017 INSTRUMENTATION

12. MAJOR PROGRESS IN SOLAR OBSERVING CAPABILITIES COINCIDES WITH ENORMOUS IMPROVEMENTS IN MAGNETO-HYDRODYNAMIC MODELING CAPABILITIES THEORY  OBSERVING SYNERGY

13. http://www.hao.ucar.edu/Profiles%20In%20Science/Rempel1.php MATTHIAS REMPEL High Altitude Observatory Boulder CO USA RESOLUTION: 16 x 16 x 12 km = > 0.022 x 0.022 arcsec TIME SPAN: 48 hours

14. OBSERVATION Swedish Solar Telescope MHD MODEL Matthias Rempel INTENSITY IMAGES

15. MAGNETIC FIELD OUTWARD FLOW

16. INTENSITY VERTICAL MAGNETIC FIELD BOB STEIN Michigan State University Lansing, MI USA RESOLUTION: 6 km = 0.008 arcsec http://steinr.pa.msu.edu/~bob/data.html

17. “RAW” (12.1-m) ATST (4-M) NST (1.6-m) SST (1-m) HINODE (0.5-m) G-BAND (431 nm) λ (μm) Nearby Line 0.86 0.854 CaII ▲( 8-m) Δ( 4-m) 3.2-m 1.29 1.083 HeI 12-m ▲ 4.8-m Δ 1.0746 FeXIII 1.72 1.548 FeI (g=3) 16-m ▲ 6.4-m Δ (4-m) 2-m ~ 1.6 H - minimum 3.44 B α (4.05) & Bβ (2.63) ▲ (8-m) Δ( 4-m) 4.80 CO Bands ▲ Δ 6.90 opaque atmosphere ▲(8-m) Δ » 12.3 MgI (3700K) ▲ »

18. “RAW” (12.1-m) ATST (4-M) NST (1.6-m) SST (1-m) HINODE (0.5-m) G-BAND (431 nm) λ (μm) Nearby Line 0.86 0.854 CaII ▲( 8-m) Δ( 4-m) 1.29 1.083 HeI ▲ Δ 1.0746 FeXIII 1.72 1.548 FeI (g=3) ▲ Δ ~ 1.6 H - minimum 3.44 B α (4.05) & Bβ (2.63) ▲ Δ 4.80 CO Bands ▲ Δ 6.90 opaque atmosphere ▲ Δ » 12.3 MgI (3700K) ▲ »

19. EFFECT OF MULTI-CONJUGATE ADAPTIVE OPTICS ESO MCAO DEMONSTRATOR * Requires Knowledge of Wavefront Distortion vs Height => Needs Atmospheric Tomography * Uses Multiple Deformable Mirrors Conjugated to Different Heights * Increases Field-Of-View by Factor 2N (diameter) or 4N 2 (N=nr of DMs) * Included in Design of All Extremely Large Nighttime and Solar Telescopes No MCAO With MCAO

20. CaII 0.86 μm FeI 1.548 μm CO Bands 4.80 μm MgI 12.3 μm. CORRECTED FIELD-OF-VIEW FOR SINGLE CONJUGATE AO (SCAO) AND TRIPLE CONJUGATE AO (TCAO) NOTES: (1) FOV is not Dependent on Telescope Diameter (2) At 12.3 µm MgI has Full Disk image with 0.3” Resolution!

21. ATMOSPHERIC TOMOGRAPHY WITH THE RING TELESCOPE

22. BEAM CROSSECTION Height 12 km λ = 1.56 µm Corrected Area: SCAO (20”) TCAO (100”) 8-meter RING TELESCOPE

23. BEAM CROSSECTION Height 12 km λ = 1.56 µm Corrected Area: SCAO (20”) TCAO (100”) 8-meter FILLED TELESCOPE

24. RING TELESCOPES REQUIRES MORE (~ 3 x) “GUIDE STARS” (= sub-areas on Sun) THAN FILLED-APERTURE TELESCOPES

25. CONCLUSIONS FOR 8-METER APERTURE CHINESE GIANT SOLAR TELESCOPE DESIGN 1. Design Telescope for Near-Infrared & Infrared Wavelengths (0.8 μm – 13 μm) 2. Note that in IR Sunspots are Less Dark and Hence Less Affected by Scattered Light 3. Allow for Future Extension to Visible Wavelengths in case MHD Models & ATST/EST Data Demand Better Resolution 4. Include Multi-Conjugate Adaptive Optics (MCAO => TCAO?) 5. Prefer Filled Aperture to Allow for Atmospheric Tomography 6. But Ring Aperture Ok but will Requires ~3x more “Guide Stars” 7. Consider Low Scattered Light at IR Wavelengths (Coronagraph) to Allow Coronal Magnetic Field Observations at High Resolution 8. Consider also Laser Guide Star SCAO or TCAO in Corona

26. WHAT ABOUT LOCATION ?? I MONGOLIA !

27. TOLBO NUUR MONGOLIA 50 km S of ÖLGII 2080 m ALTITUDE 3 x 20 km SIZE FRESH WATER

28. TOLBO NUUR 2080 m HIGH 3 x 20 km URUMQI

31. Figure 7. Daily mean distribution per month of probable NAOH (number of astronomical observation hours) for three Mongolian sites and for two sites in Middle Asia. Circles: Khureltogot, +:Dalanzadgad, ×: Muren,squares: Khairabad, triangles: Sanglock.Figure reference:[1]. References [1] Batsukh G, Ganbaatar D, Khaltar D and Tugjisuren N 1995, A&ASS 113 341 NIGHTTIME! HOURS!

32. THE END