initial results of eis shinsuke imada (naoj) eis team
TRANSCRIPT
Initial Results of EIS
Shinsuke Imada (NAOJ)
EIS Team
HINODE Spacecraft• HINODE (which was called
SOLAR-B before launch) was successfully launched on 23 Sep, 2006.
• Observations started from the beginning of Nov 2006.
SOT
XRT
EIS
The Instrument
• Wavelength bands170Å-210Å250Å-290Å
• Slits & slots1”, 2”, 40”, and 266”
• High resolutions0.0223Å/pixel & 1”/pixel
• High throughputMinimum number of reflectionMulti-layer coating of the mirrorSuitable for transient phenomena
Field of View
E
S
EIS (576”x512”)
XRT(2048”x2048”)
W
SOT:NFI/SP(328”x164”)SOT: BFI
(205”x102”)
N
Young et al (2007)
Cold lines < 1MK
HeII: 256.3 A (T=4.9)
OV: 192.9 A (T=5.4)
MgV: 276.6 A (T=5.4)
FeVIII: 185.1 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)
Hot lines >1MK
FeXI: 188.2 A (T=6.1)
SiX: 261.0 A (T=6.1)
FeXII: 195.1 A (T=6.1)
FeXIII: 202.0 A (T=6.2)
FeXIV: 264.8A (T=6.3)
FeXV:284.2A(T=6.3)
FeXVI:263.0A(T=6.4)
Emission Measure
Watanabe et al (2007)
QUIET SUN
Active RegionFlare
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
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.
Active Region Footpoint
Hara et al (2007)
Exploring North Pole• Soft X-ray image shows many Ioop-shaped bright
points in coronal hole
EIS FOV
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)
Culhane et al (2007)
Jet 1
• Light curve show the Typical Jet time profile.
• Intensity rise at 15:10, and reduce slowly.
Jet2
• Light curve show Two peaks.
• Hot plasma eject from bright point at ~16:35.
• Middle temperature plasma are come back to BP.
Flare Observation Dec13th 2006
02:00 03:00
EIS Observation
Filament rotation
Williams et al (2007)
VelocityIntensity
Please note that this is observed before X-class Flare!! Trigger??
Ejection at impulsive phaseAsai et al (2007)
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
Temperature-Dependent Upflow
Upflow velocity is clearly depend on its temperature.
The trend on temperature is dramatically changed ~1MK.
Dec 14th Flare
Harra et al (2007)
LDE Flare Event He II 256 Fe XII 195 Fe XV 284 Ca XVII/Fe XI 192
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!