1. Direct Evidence of Emergence of a Helical Flux Rope under an Active- Region Prominence Joten Okamoto Kyoto Univ. ／ NAOJ JSPS Research Fellow Saku Tsuneta, Bruce Lites, Masahito Kubo, Takaaki Yokoyama and Japan-US Hinode/SOT team + KD Leka, Tom Metcalf This work is my PhD thesis topic. I am provided limited protection for the data sets. (see http://solarb.msfc.nasa.gov/for_scientists/topics.html, http://solar-b.nao.ac.jp/hsc_e/OnGoing_top.shtml )http://solarb.msfc.nasa.gov/for_scientists/topics.htmlhttp://solar-b.nao.ac.jp/hsc_e/OnGoing_top.shtml I have submitted the former part of this work to ApJL. The latter part (not included in this PPT) will be submitted.

2. Hinode satellite Hinode was launched in Sep. 2006. 3 instruments SOT (Soalr Optical Telescope) –photosphere, chromosphere XRT (X-ray Telescope) –corona EIS (EUV Imaging Spectrometer) –transition region, corona Advantage of Hinode Continuous high-quality movie Small scale structures and time variation of solar phenomena granules, small magnetic elements, spicules, prominences, … In this talk, we focus on prominence observation. SOT EIS XRT

3. Prominence Cool plasma in the corona ~ 10,000 K over polarity inversion lines (PILs) “filament” on disk supported by coronal magnetic filed lines Questions about prominences Formation process supply of mass construction of magnetic field Fine structures and their evolution Disappearance and eruption Coronal Mass Ejection (CME) SMART Hα image (Hida Obs.) Hinode/SOT Ca II H movie （ Okamoto et al. 2007)

4. Structure of prominence magnetic fields Helical in many cases Measurement with polarization e.g., Tandberg-Hanssen, Leroy Extrapolation from eruption e.g., CME taken by SOHO/LASCO How to make this ? same or difference of QS and AR prominences ? AR prominence QS prominence prominence helical field line Prominence in the unified model of flares and CMEs (Shibata et al.)

5. Formation of prominence magnetic fields Theory Helical flux rope emergence from the photosphere e.g., Rust, Kumar, Low, Lites… Shear motion on the photosphere and reconnection in the corona e.g., Pneuman, van Ballegooijen, Martens, Antiochos, Aulanier, Karpen… Observation No clear evidence lack of accuracy of polarimetric measurement due to seeing restriction to long-duration observation How are they made ? KEY: Motion and time-evolution of magnetic field on the photosphere Tracking of evolution of AR prominence prominence helical field line

6. Data Continuous observation of AR 2007 Apr 28 ～ May 2 AR 10953 wavelength (Hinode) SpectroPolarimeter (SP) fast map (160”x160”, 3 ～ 6-hour cadence ) Hα (160”x160”, 1-min cadence) G-band 、 Ca II H (108”x108”, 1-min cadence) X-ray (512”x512”, 1-min cadence) Estimation of magnetic field Milne-Eddington inversion (Yokoyama et al.) 180°ambiguity solution with AZAM (Lites et al.) （ Current 3,4 (Metcalf et al.) ） H-alpha Ca II H ROI

7. Hα movie with Hinode/SOT deformation Hinode/SOT Hα formation Repetition of formation and deformation during 2 days 04.28 11:5604.28 23:1404.29 12:0904.29 18:1304.29 20:51 deformation formation

8. After that… （ Hida/SMART Hα ） Formation of a clear prominence it looks stable after May 1 05.01 22:27 05.02 21:1805.03 22:0905.04 21:4404.29 22:10 What can we see in SP data ? Evolution of photospheric magnetic field near the PIL during the promninence formation SOT FOV

9. （ conclusion ） Helical flux rope emergence Observational results (on the PIL) Changing direction of horizontal magnetic field Simultaneous appearance of a region having weak vertical magnetic field Simultaneous upflow in the same region plage sunspot side × Interpretation （ cross section of photosphere) × × photosphere PIL Result （ photosphere ） －＋ plagesunspot side －＋－＋ PIL

10. magneto- gram （ 1/9 ） 2007.04.29 11:43 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz plage （＞ 500 G ） PIL sunspot side （＜－ 500 G ）

11. 2007.04.29 15:36 magneto- gram （ 2/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

12. 2007.04.29 20:16 magneto- gram （ 3/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

13. 2007.04.30 01:00 magneto- gram （ 4/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

14. 2007.04.30 05:07 magneto- gram （ 5/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

15. 2007.04.30 08:56 magneto- gram （ 6/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

16. 2007.04.30 15:46 magneto- gram （ 7/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

17. 2007.04.30 22:46 magneto- gram （ 8/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

18. 2007.05.01 08:16 magneto- gram （ 9/9 ） vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： boundary of ±500G of Bz

19. 2007.04.29 11:43 2007.04.29 15:36 2007.04.29 20:16 2007.04.30 05:07 2007.04.30 15:46 2007.05.01 08:16 2007.05.01 02:06 2007.04.30 22:46 2007.04.30 08:56 vertical mag. （ color contour ）＋ horizontal mag. （ arrows ） 15” ~ 10,000 km ① ② ③ ④ ⑤ ⑥ ⑦ ⑧ ⑨

20. 2007.04.29 11:43 2007.04.29 15:36 2007.04.29 20:16 2007.04.30 05:07 2007.04.30 15:46 2007.05.01 08:16 2007.05.01 02:06 2007.04.30 22:46 2007.04.30 08:56 vertical velocity of magnetic components by ME fitting （ color contour ）＋ horizontal mag. （ arrows ） － 300 m/s ① ② ③ ④ ⑤ ⑥ ⑦ ⑧ ⑨

21. 2007.04.28 21:26 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL normal or inverse ? （ 1/12 ） normal inverse 度

22. 2007.04.29 03:46 normal or inverse ? （ 2/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

23. 2007.04.29 11:43 normal or inverse ? （ 3/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

24. 2007.04.29 15:36 normal or inverse ? （ 4/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

25. 2007.04.29 20:16 normal or inverse ? （ 5/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

26. 2007.04.30 05:07 normal or inverse ? （ 6/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

27. 2007.04.30 08:56 normal or inverse ? （ 7/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

28. 2007.04.30 12:46 normal or inverse ? （ 8/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

29. 2007.04.30 15:46 normal or inverse ? （ 9/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

30. 2007.04.30 22:46 normal or inverse ? （ 10/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

31. 2007.05.01 02:06 normal or inverse ? （ 11/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

32. 2007.05.01 05:16 normal or inverse ? （ 12/12 ） normal inverse 度 vertical mag. red ：＋ blue ：－ horizontal mag. arrows black line ： PIL

33. Helical flux rope emergence Observational results (on the PIL) Changing direction of horizontal magnetic field Simultaneous appearance of a region having weak vertical magnetic field Simultaneous upflow in the same region plage sunspot side × Interpretation （ cross section of photosphere) × × photosphere PIL Result （ photosphere ） －＋ plagesunspot side －＋－＋ PIL

34. Helical flux rope emergence Result （ photosphere ） －＋ plagesunspot side －＋－＋ PIL

35. Emergence of helical flux rope and Prominence 2007.04.29 20:16 2007.04.30 05:07 2007.04.30 08:56 2007.04.29 15:36 Continuous prominence appeared after the emergence of the flux tube Some remnants of prominence existed before the event The newly-emerging fields connect with original fields or get rid of those ?

36. Motion on the photosphere （ G-band ） 2007.04.30 08:56 Red circle indicates the orientation of the prominence

37. advective flow: arrows 2007.04.30 08:56 No clear sheared motion, but some mesogranules under the prominence = support to emergence ? Red circle indicates the orientation of the prominence Motion on the photosphere （ G-band ）

38. Physical parameters plage （＋） PILsunspot side （－） Bz (G) ＋ 1100 ±400 0 ±200 － 1000 ±400 Bxy (G) 400 ±200 650 ±150 650 ±200 Vz (m/s) ＋ 200 ±500 － 300 ±200 － 100 ±700 filling factor 0.23 ±0.20 0.15 ±0.05 0.30 ±0.20 Mag. field strength of prominence: ～ 100 G 650 G ×0.15 10,000 km 2007.04.30 05:07 plage PIL sunspot side Duration of emergence ： 24 – 36 hours Rising height ： ～ 25,000 km 24 h ×300 m/s

39. Summary Clear evidence of emerging helical flux rope associated with formation of prominence Appearance of magnetized region that had weaker field strength along the PIL After that, prominence was stabilized No continuous sheared motion along the PIL Shear/reconnection model is ruleed out ?... No Our result is one example in an active region Necessary to observe active/quiescent prominences quantitatively How to emerge ? Possible to emerge a whole long rope whose length is several tens of thousand km ? Why is it located along the PIL ? Mechanism of mass supply ? … We don’t know. It supplied only helical magnetic field to the corona.