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!