Observations and Modelings of the Solar Flux Emergence

Transcription

1 Observations and Modelings of the Solar Flux Emergence Shin Toriumi (Univ. of Tokyo) Supervisor: T. Yokoyama (U. Tokyo) Hinode- 7 (2013 Nov. 13)

2 1. IntroducEon AIA 335 AIA 171 AIA 304 HMI Cont. HMI Mag. NASA/SDO

3 1. IntroducEon Numerical SimulaEon: Emergence from - 20 Mm Mag. field: log ( B /B 0 ) Toriumi & Yokoyama (2012)

4 1. IntroducEon Importance of Flux Emergence Transports the magneec flux from the deep interior Creates aceve regions SomeEmes causes erupeons such as flares and CMEs ObservaEonal and Numerical studies

5 2. Emergence in the Deep Interior Importance of Flux Emergence Transports the magneec flux from the deep interior Creates aceve regions SomeEmes causes erupeons such as flares and CMEs ObservaEonal and Numerical studies

6 2. Emergence in the Deep Interior Numerical SimulaEons Thin- flux- tube appoximaeon (Spruit 1981) B eq at the bo[om of the CZ: at least 10 4 G Total flux of ARs: Mx Cross- seceonal size of the tube: ~1,000 km Pressure scale height: a few 10,000 km AnelasEc approximaeon (Gough 1969) EquaEon of conenuity is approximated by! "(! 0 V) = 0 Flux tube is thin Sound waves are filtered out

7 2. Emergence in the Deep Interior Numerical SimulaEons Thin- flux- tube appoximaeon (Spruit 1981) Field strength of 10 5 G is required for the tubes to emerge at sunspot laetudes Colioris force is responsible for various asymmetries between the leading and following polariees AnelasEc approximaeon (Gough 1969) Emergence in the rotaeng spherical shell Retrograde flow along the flux tube Emergence in the conveceve interior Caligari et al. (1995) Fan (2008)

8 2. Emergence in the Deep Interior ObservaEonal Studies Probing by Local Helioseismology A B Ilonidis et al. (2011) l Time- distance helioseismology C D l Detected seismic anomaly in the deep conveceon zone at ~- 65 Mm l Up to 2 days before the flux emergence a[ains its peak flux growth rate Ilonidis et al. (2011) l Rising velocity: km s - 1

9 3. Birth of AcEve Regions Importance of Flux Emergence Transports the magneec flux from the deep interior Creates aceve regions SomeEmes causes erupeons such as flares and CMEs ObservaEonal and Numerical studies

10 3. Birth of AcEve Regions 5- day ObservaEon of AR 11130: Small- scale Features

11 3. Birth of AcEve Regions ResisEve Emergence Process SuggesEon of the Model (Pariat et al. 2004) Photospheric fields have serpenene structure (Strous & Zwaan 1999) Local flux cancellaeons of these fields Ellerman bombs Later simulated by Isobe et al. (2007) and ArchonEs & Hood (2009) Fig. 9. Sketch of the field Pariat lines overlying et al. the (2004) emerging flux. Toriumi et al. (2012)

12 3. Birth of AcEve Regions ResisEve Emergence Process ConvecEve emergence (Cheung et al. 2010) CancellaEons coupled with conveceon remove mass from the surface layer Key process for enere tube emergence Cheung et al. (2010)

13 3. Birth of AcEve Regions ResisEve Emergence Process Spectroscopy (Matsumoto et al. 2008) ObservaEon of an Ellerman bomb Upflow of 1-3 km s - 1 in the chrom. Downflow of 0.2 km s - 1 in the photo. Bi- direceonal jet due to reconneceon Hα- 0.8 Hα+0.8 MDI Magnetogram ConEnuum Matsumoto et al. (2010)

14 3. Birth of AcEve Regions ResisEve Emergence Process Future ObservaEon Hinode and Solar- C Spectro- Polarimetry : SOT and SUVIT Scan the emerging flux region at the photosphere and the chromosphere To quanetaevely invesegate the contribueon of each process to the enere flux tube emergence Chrom. Photo.

15 1. IntroducEon Importance of Flux Emergence Transports the magneec flux from the deep interior Creates aceve regions SomeEmes causes erupeons such as flares and CMEs ObservaEonal and Numerical studies

16 4. FormaEon of a Flaring AcEve Region Flaring AR: NOAA Produced a series strong flares including X2.2- class event Highly sheared PIL in the central δ- sunspots Hinode/SOT : movie courtesy of T. Okamoto

17 4. FormaEon of a Flaring AcEve Region Previous Studies Kusano et al. (2012) ReconnecEon between the sheared coronal arcades Sammis et al. (2000) δ- sunpots produce many more large flares Max. X- Ray Flux Spot Group Area

18 4. FormaEon of a Flaring AcEve Region ì Previous Studies ì Kusano et al. (2012) Sammis et al. (2000) PIL, coronal δ- sunspots ì Sheared ReconnecEon between the arcade, and ì δ- sunpots produce many coronal arcades more large flares ü sheared Important for produceon of intensive flares ì No. 1, 2000 RELATION BETWEEN d SPOTS AND LARGE FLARES Max. X- Ray Flux What creates such structures in an AR? ü FormaEon of AR from the flux emergence ü Target region : AR Spot Group Area FIG. 2.ÈPeak Ñare intensities in W m~2 for each spot group as a function of peak area in disk fraction, with each magnetic class plotted separ

19 4. FormaEon of a Flaring AcEve Region EvoluEon of AR Composed of two emerging bipoles P1- N1 and P2- N2 Sheared PIL is created between N1 and P2, which forms δ- sunspots

20 4. FormaEon of a Flaring AcEve Region Photospheric EvoluEon 1. P1- N1 / P2- N2 appear at the surface N1 P1 N2 P2

21 4. FormaEon of a Flaring AcEve Region Photospheric EvoluEon 1. P1- N1 / P2- N2 appear at the surface 2. P2 driss along the southern edge of N1, forming a sheared PIL Sheared PIL N2 P2 N1 δ- sunspots P1

22 4. FormaEon of a Flaring AcEve Region N2 Coronal EvoluEon 3. Coronal arcade conneceng N1- P2 is then created above the PIL 4. A series of strong flares (including X and M events) occur at this PIL P2 N1 P1 y [pixels] y [pixels] GOES SXR [W m -2 ] (a) 12-Feb :15 UT (b) N2 N1 P x [pixels] (e) N2 N1 P2 P M6.6 (c) 13-Feb :00 UT N x [pixels] M2.2 02/ Date (d) SDO/AIA 171 X2.2 P2 X M C

23 4. FormaEon of a Flaring AcEve Region FormaEon of AR Two possible scenarios for this AR Case 1 Case 2 N1 N1 P1 P1 N2 P2 N2 P2 L Emergence of a single split tube L L Emergence of two independent tubes L

24 4. FormaEon of a Flaring AcEve Region FormaEon of AR D MHD simulaeon of magneec flux tubes for Cases 1 and 2 Case 1 Case z/h x/h x/h y/h 0 Mimic the spliung by sinking the middle part Length: H 0 = 200 km Time: τ 0 = 25 s Field strength: B 0 = 300 G

25 4. FormaEon of a Flaring AcEve Region FormaEon of AR Results: Magnetogram Case 1 : single split tube Case 2 : two independent tubes

26 4. FormaEon of a Flaring AcEve Region FormaEon of AR Results: Magnetogram Case 1 : single split tube Arrows: B h Sheared PIL N1 P2 Case 2 : two independent tubes δ- sunspots

27 4. FormaEon of a Flaring AcEve Region FormaEon of AR Results: Coronal fields and reconneceon Case 1 (t/τ 0 = 120) 1. P1- N1 and P2- N2 come closer to the middle of the region. 2. ReconnecEon occurs in a current sheet. 3. Arcade field (N1- P2) is created, while post- reconneceon field (P1- N2) is ejected upward. N1 P2 N2 P2 N1 P1

28 4. FormaEon of a Flaring AcEve Region FormaEon of AR Results: Coronal fields and reconneceon Case 1 (t/τ 0 = 120) 1. P1- N1 and P2- N2 come closer to the middle of the region. 2. ReconnecEon occurs in a current sheet. 3. Arcade field (N1- P2) is created, while post- reconneceon field (P1- N2) is ejected upward. N1 P2 N2 P2 N1 P1

29 4. FormaEon of a Flaring AcEve Region Comparison of the ObservaEon and SimulaEons CreaEon of the sheared PIL

30 4. FormaEon of a Flaring AcEve Region Comparison of the ObservaEon and SimulaEons CreaEon of the sheared PIL (a) AR (b) Case 1 (c) Case In AR 11158, N1 P2 vector rotates and the length becomes shorter. Only Case 1 shows a similar trend. In Case 2, N1 and P2 simply fly by.

31 4. FormaEon of a Flaring AcEve Region FormaEon of AR Conclusion: Case 1 is more likely the case Case 1 Case 2 N1 N1 N2 P2 P1 N2 P2 P1 L Emergence of a single split tube L L Emergence of two independent tubes L

32 4. FormaEon of a Flaring AcEve Region FormaEon of AR Conclusion: Case 1 is more likely the case Case 1 N2 P2 N1 P1 Two emerging fields of AR shared a common root below the surface. Emergence of single tube produced Sheared PIL and coronal arcade δ- sunspots which is responsible for the flares L Emergence of a single split tube L Large- scale flux emergence is greatly responsible for the flaring aceviees.

33 5. Summary Flux Emergence from the Interior to the Atmosphere Emergence in the Deep Interior SimulaEons Helioseismology Birth of AcEve Regions Small- scale features ResisEve emergence model Hinode / Solar- C FormaEon of a Flaring AcEve Region Depth / Height Sheared PIL, coronal arcade, and δ- sunspots AR 11158: single split tube rather than two tubes Large- scale emergence is responsible for the flare aceviees (Toriumi et al., submi[ed) TIme

34 Thank you for your attention!