Presentation is loading. Please wait.

Presentation is loading. Please wait.

Initial Results of EIS Shinsuke Imada (NAOJ) EIS Team.

Similar presentations


Presentation on theme: "Initial Results of EIS Shinsuke Imada (NAOJ) EIS Team."— Presentation transcript:

1 Initial Results of EIS Shinsuke Imada (NAOJ) EIS Team

2 HINODE Spacecraft HINODE (which was called SOLAR-B before launch) was successfully launched on 23 Sep, Observations started from the beginning of Nov SOT XRT EIS

3 The Instrument Wavelength bands 170Å-210Å 250Å-290Å Slits & slots 1”, 2”, 40”, and 266” High resolutions Å/pixel & 1”/pixel High throughput Minimum number of reflection Multi-layer coating of the mirror  Suitable for transient phenomena

4 Field of View E S EIS (576”x512”)‏ XRT (2048”x2048”)‏ W SOT:NFI/SP (328”x164”)‏ SOT: BFI (205”x102”)‏ N

5 Young et al (2007) ‏ Cold lines < 1MK HeII: A (T=4.9) OV: A (T=5.4) MgV: A (T=5.4) FeVIII: A (T=5.6) MgVI: 269.0A (T=5.6) MgVII:278.4A(T=5.8) SiVII:275.4A(T=5.8) FeX:184.5A(T=6.0)

6 Hot lines >1MK FeXI: A (T=6.1) SiX: A (T=6.1) FeXII: A (T=6.1) FeXIII: A (T=6.2) FeXIV: 264.8A (T=6.3) FeXV:284.2A(T=6.3) FeXVI:263.0A(T=6.4)

7 Emission Measure Watanabe et al (2007) ‏ QUIET SUN ‏ Active Region ‏ Flare

8 Active Region Multi-Temperature Structure of active region. ‏ One may find that High-Temperature loops are wider than Low-Temperature loops!! 0.4 MK ‏ 2.5 MK ‏

9 Loop Width Brooks et al (2007) ‏ The loop width is clearly depend on plasma temperature. This result is very interesting, because plasma beta is very low in solar corona.

10 Active Region Footpoint Hara et al (2007) ‏

11

12 Exploring North Pole Soft X-ray image shows many Ioop-shaped bright points in coronal hole EIS FOV

13 Reconnection Jet Flux emerging in open field structure can produce jets. Line of sight velocity: 30km/s Taking account of projection effect, actual velocity could be much higher ( > 300 km/s) ‏ Is the jet connecting to solar wind? + Kamio et al (2007) ‏

14 Culhane et al (2007) ‏

15 Jet 1 Light curve show the Typical Jet time profile. Intensity rise at 15:10, and reduce slowly.

16 Jet2 Light curve show Two peaks. Hot plasma eject from bright point at ~16:35. Middle temperature plasma are come back to BP.

17 Flare Observation Dec13th :00 03:00

18 EIS Observation

19 Filament rotation Williams et al (2007) ‏ Velocity Intensity Please note that this is observed before X-class Flare!! Trigger??

20 Ejection at impulsive phase Asai et al (2007) ‏

21 Doppler Shift (Velocity) map FeXV FeX FeXII HeII FeXIII FeXIV ~ 4.5 hour > 1 hour Imada et al (2007) ‏ The upflows are observed at boundary of Transient Coronal Hole in Plage region at gradual phase of X-class flare. 150km/sec -150km/sec

22 Temperature-Dependent Upflow Upflow velocity is clearly depend on its temperature. The trend on temperature is dramatically changed ~1MK.

23 Dec 14 th Flare Harra et al (2007) ‏

24 LDE Flare Event He II 256Fe XII 195 Fe XV 284Ca XVII/Fe XI 192

25 EIS Summary EIS works perfectly!! EIS observe many new solar aspects for Active region Polar coronal hole Flare Thank you very much for your attention!

26


Download ppt "Initial Results of EIS Shinsuke Imada (NAOJ) EIS Team."

Similar presentations


Ads by Google