ABSTRACT(In Alphabetical Order of Author Names)

Strongly Blueshifted Phenomena Observed in a Flare with Hinode/EIS
A. Asai1 , H. Hara1 , T. Watanabe1 , S. Kamio1 , S. Imada1 , N. Narukage2 , and T. Sakao2(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
We present a detailed examination on strongly blueshifted phenomena observed with the Extremeultraviolet Imaging Spectrometer on board the Hinode satellite associated with an X3.4 flare that
occurred on 13 December 2006. We discuss physical characteristics of the phenomena by comparing
the Hinode SOT and XRT data.

9A New View of Coronal Magnetic Topology From the Hinode XRT
E.E. DeLuca, L. Golub, G. Aulanier, and A.A. van Ballegooijen
Smithsonian Astrophysical Observatory
The combination of broad temperature sensitivity, high spatial resolution and large dynamic range
allows the X-ray Telescope (XRT) on Hinode to observe the magnetic connectivity from the core ofactive regions to the quiet sun, and to follow the dynamic changes in that connectivity. For the firsttime we see the entire structure within an active region, not just the loop tops or footpoints. Relating
the coronal structure and dynamics to the evolution of the photospheric magnetic field is a primary
goal of the Hinode mission. We present X-ray observations in support of that goal.

10

Interaction between Non-Thermal Electrons and Plasma
in the Chromosphere and Transition Region during Solar Flares:
Energetic Balance of Solar Flares
R. Falewicz1 , P. Rudawy1 , and M. Siarkowski2(1) Astronomical Institute, University of Wroclaw(2) Space Research Center, Polish Academy of Sciences
The main aim of our investigations is the interaction between non-thermal electrons and plasma inflaring loops and the energetic balance of solar flares. Taking into account the influence of the energy
spectrum of non-thermal electrons speeding down the flaring loops, the geometry of the loops, properties of the plasma (density, temperature) we intend to explain the processes of plasma evaporationand the formation of the observed chromospheric emission in strong Fraunhofer lines (like Hα, calcium
lines etc.).
In our investigations we plan to use: SXR images taken with XRT telescope on board the Hinodesatellite, HXR data taken with RHESSI, narrow and broadband data taken with the Solar Optical
Telescope (Hinode/SOT), high-temporal resolution optical spectra taken with ground-based telescopes(MSDP spectrograph with SECIS instrument of the Wroclaw Observatory and THEMIS telescope).
Using observational data we will investigate the total energy balance of flaring loops. Our goalis the explanation of how the energy spectrum of non-thermal electrons and the structure of flaring
loops affect the processes of interaction of electrons with chromospheric and coronal plasma and theprocesses of evaporation. This analysis will use corresponding codes for numerical modeling of thechromospheric and corona emission.
The project is still under development and the collaboration with various scientific teams is kindly
appreciated.

11

Microwave Enhancement in Coronal Holes
N. Gopalswamy1 and K. Shibasaki2(1) NASA/Goddard Space Flight Center(2) Nobeyama Solar Radio Observatory, NAOJ
The microwave enhancement in coronal holes is a unique radio signature different from what is observed
at other wavelengths. In microwaves, coronal holes appear bright over a narrow frequency range above≈ 15 GHz. The enhancements are readily imaged by the Nobeyama radioheliograph at 17 GHz bothin the polar and equatorial holes. Compact brightpoints that are observed in the coronal holes aredifferent from the coronal brightpoints and correspond to the network junctions. These bright points
often show flare-like brightenings. It has been suggested that the radio enhancement reflects the
dynamic nature of the chromosphere because the thermal radio emission at 17 GHz originates fromthe upper chromosphere where the temperature is around 10 000 K. The enhancement is seen as afew percent increase in the brightness temperature over the quiet chromospheric values. Combined
17 GHz and Hinode observations are likely to help make progress on this phenomenon. Since coronalholes are the seats of high speed solar wind, the coronal holes may provide some clue to the solar windorigin. High-speed streams are also important for causing geomagnetic storms if they are directed at
Earth.
This paper is dedicated to the memory of Professor T. Kosugi

122006 Dec 17 Long-Duration Flare Observed with Hinode EIS
H. Hara1 , T. Watanabe1 , L.K. Harra2 , J.L. Culhane2 , P.J. Cargill3 , G.A. Doschek4 , and
J.T. Mariska4(1) National Astronomical Observatory of Japan(2) Mullard Space Science Laboratory(3) Space and Atmospheric Physics, Imperial College London(4) Naval Research Laboratory
Long-duration solar flares generally have a cusp apex at the loop top. The cusp shape reflects the
topology of magnetic fields near the flare-loop top and it is one of the indirect pieces of evidence
supporting the occurrence of the magnetic reconnection process above flare loops. The Hinode EUV
Imaging Spectrometer (EIS) observed a long-duration flare that occurred on 2006 Dec 17. We present
the first EIS spectroscopic observation of cusp-shaped flare loops. We also report velocity fields aroundthe cusp structures and post-flare loops.

13

High-Velocity Nonthermal Plasma Motion Concentrated at
the Footpoints of Coronal Loops
H. Hara1 , T. Watanabe1 , L.K. Harra2 , P.R. Young3 , G.A. Doschek4 , and J.T. Mariska4(1) National Astronomical Observatory of Japan(2) Mullard Space Science Laboratory(3) Rutherford Appleton Laboratory(4) Naval Research Laboratory
Hinode EUV imaging spectrometer has observed large line widths in the EUV coronal emission lines
near the footpoints of coronal loops. It is highly suggestive that the heating of coronal loops is taking
place near the footpoints.

14

Coronal Dimming Observed with Hinode
L.K. Harra1 , H. Hara2 , P.R. Young3 , D.R. Williams1 , A.C. Sterling4 and G.D.R. Attrill1(1) Mullard Space Science Laboratory(2) National Astronomical Observatory of Japan(3) Rutherford Appleton Laboratory(4) Naval Research Laboratory(4) NASA/Marshall Space Flight Center
Coronal dimming has been a technique used to determine the source of plasma that forms part of acoronal mass ejection. Generally dimming is detected through imaging instruments such as SOHOEIT by taking difference images. In a few cases the SOHO-CDS has been used to determine outflowing
material, and a decrease in density. Hinode tracked active region 10930 from which there were a seriesof flares. We combine dimming observations from EIT with Hinode data to show the impact of flaresand coronal mass ejections on the region surrounding the flaring active region, and we discuss evidence
that the eruption resulted in a prolonged steady outflow of material from the corona.

15

Temperature Diagnosis of Coronal Loop Oscillations Using Hinode EIS andNorikura NOGIS Coronagraph
K. Hori, K. Ichimoto, T. Sakurai, and EIS & NOGIS Teams
National Astronomical Observatory of Japan
NOrikura Green-line Imaging System, “NOGIS” (Ichimoto et al. 1999), is a 10cm-aperture coronagraph developed at the Norikura Solar Observatory, NAOJ. Using a 5303 Å (Fe xiv) Lyot filter,
NOGIS can provide both intensity and Doppler velocity images of 2 MK plasma from the coronalgreen-line emission. The Doppler images are constructed by subtracting a [λ − 0.45 Å] image from a[λ + 0.45 Å] image. The line-of-sight velocity up to ±25 km s−1 can be obtained with an accuracy of
about 0.6 km s−1 . NOGIS field of view is 2000 × 2000 pixels in a full frame mode. Spatial resolution is
1.84 arcseconds in a partial frame mode and time resolution is reduced to about 1 minute to increasesignal-to-noise ratio.
Since July 1997, NOGIS has observed many coronal transients in the inner corona (up to 1.5
R ), such as flares, plasma ejections, propagating waves and loop oscillations (Yamasaki 2001; Horiet al. 2005; Suzuki et al. 2005). Because the NOGIS observation is restricted to emission from
2 MK plasma, it is difficult to examine the heating/cooling processes in the individual events. We
propose a NOGIS joint observation with Hinode EIS and XRT, especially for temperature diagnosis ofcoronal loop oscillations above the solar limb. The existence of temperature dependency in flare loop
oscillations is already reported from SOHO/SUMER slit observations. We expect that combinationof Hinode/EIS and NOGIS can detect loop oscillations even in “apparently” quiet loops. If such
oscillations commonly exist through the corona, their damping energy can be counted as one ofcoronal heating sources. Detailed observation plan will be presented. (N.B. NOGIS observation will
be resumed in the beginning of May in this year.)16

Diagnosis of Fine Structures in Solar Radio Bursts as Manifestation ofMagnetic Reconnection Processes
J. Huang and Y. Yan
National Astronomical Observatories, Chinese Academy of Sciences
Solar radio emission in cm and dm wave range plays an important role in understanding energy
release, plasma heating, particle acceleration and particle transport during solar bursts. With thehigh time and temporal resolution (4 MHz in 1.25 ms) mode of Huairou Solar Broadband Radio
Dynamic Spectrometer in 1.100 – 1.340 GHz, we have observed lots of new fine structures of solar
radio bursts during the flares and other solar activities. We present the observations on 1 December
2004, which exhibit plenty of radio fine structures. Among them, a hand-shaped burst that occurred
during the impulsive phase is interesting. This group of bursts showed a unique fine structure with
mixed fast-and-slow frequency drift rate. We suppose that its fast, positive-frequency drift may be
due to the fast downward flows from the reconnection site and its slow, negative-frequency drift may
be due to the slow upward motion of flare loops.
Our radio spectrometer data give information on the core region of the reconnection site. Hinodewill provide us with data of the Sun’s three-dimensional magnetic fields, monochromatic images ofvarious wavelengths, and the X-ray images. The Chinese Spectral Radioheliograph will give imagesof solar bursts at 500 MHz – 15GHz bands. All of them being combined, we will be able to obtainbetter understanding on the physics of solar radio bursts.

17

Flare Energy and Fast Electrons via Alfvén Waves
H.S. Hudson1 and L. Fletcher2(1) Space Sciences Laboratory, University of California, Berkeley(2) Department of Physics and Astronomy, University of Glasgow
The impulsive phase of a solar flare marks the epoch of rapid conversion of energy stored in the preflare coronal magnetic field. Hard X-ray observations imply that a substantial fraction of flare energy
released during the impulsive phase is converted to the kinetic energy of mildly relativistic electrons(10 – 100 keV). We investigate a new scenario, intended to replace the “thick target model,” in which
shear Alfvén waves transport the energy from its coronal sources and at the same time generate
fast electrons either directly, via inertial effects in the corona, or indirectly via a turbulent cascade
developing in the chromosphere. This scenario offers solutions to some perplexing flare problems,such as the flare “number problem” of finding and resupplying sufficient electrons to explain theimpulsive-phase hard X-ray emission.

18

Searching for Umbral Dots in Hinode Data
N.E. Hurlburt, Ralph Seguin, S.L. Freeland, and the SOT Team
Lockheed-Martin Solar and Astrophysics Laboratory
We present an approach for finding and analysing observations taken by the Solar Optical Telescope(SOT) on Hinode by conducting a study of umbral dots. The observations consist of coordinated,
multi-wavelength observing sequences spanning several hours for each spot considered. Typically these
multi-wavelength observations include longitudinal magnetograms in 6302 Å, and filtergrams in Ca ii
H, G-band and blue continuum. Various tools and techniques will be presented that will be used aspart of the investigation.

19

Fine Structures of the Evershed Flow Observed by SOT aboard HinodeK. Ichimoto1 , Y. Suematsu1 , S. Tsuneta1 , Y. Katsukawa1 , M. Shimojo1 , M. Kubo2 , T. Shimizu2 ,R.A. Shine3 , T.D. Tarbell3 , A.M. Title3 , B.W. Lites4 , D.F. Elmore4 , T. Yokoyama5 , and S. Nagaka6(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Lockheed-Martin Solar and Astrophysics Laboratory(4) High Altitude Observatory, NCAR
(5) Department of Earth and Planetary Science, University of Tokyo(6) Kwasan and Hida Observatories, Kyoto University
Small scale structure of the Evershed effect was studied using the Spectropolarimeter (SP) and Broadband Filter Imager (BFI) of SOT aboard Hinode. SP maps and high cadence continuum images of BFIcovering the entire sunspots are used to investigate the spatial distribution of the flow field, brightness
and magnetic fields. It is revealed that the Evershed flow starts at the front edge of inwardly migrating
penumbral grains with an upward velocity component and turns to nearly horizontal flow preferentially in dark lanes (or dark core of filaments) of the penumbra. Our results are in general agreementwith the well known un-combed penumbral concept in which the Evershed flow takes place in nearlyhorizontal field channels. We discovered a number of tiny elongated regions in the deep photospherein which there is an obvious upward motion of 1 – 1.5 km s−1 distributing over the penumbra. They
could be identified as the ‘foot points’ of the individual Evershed flow channels. Cross-correlation
among the flow speed, intensity, magnetic field strength and inclination, and distribution of strong
down flows in and around the penumbra will also be discussed.

20

Temperature-Dependent Upflow in the Plage Associated with an X3.2 Flareon 13 December 2006
S. Imada1 , H. Hara1 , T. Watanabe1 , A. Asai1 , S. Kamio1 , K. Matsuzaki2 , and EIS Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
We present Hinode/EIS raster scan observations of a plage region taken during the gradual phaseof an X3.2 flare of 13 December 2006. The plage region is located 200 arcsec eastward from theflare arcade. The spectral observations with multi-wavelengths allow us to determine velocities fromthe Doppler shifts in various temperatures. EIS observed strong upflows in addition to a stationary
plasma in the Fe xv line 284.2 Å (log T = 6.3) in the plage region. The strong upflows are almost 160
km s−1 which is calculated by two component Gaussian fitting. On the other hand, at the transition
region temperature (He ii 256.3 Å, log T =4.7), very weak upflows, almost motionless, were observed.
Furthermore, we found that these upflow velocities clearly depend on the temperature, by comparing
the upflow velocities among Fe xv, Fe xiv, Fe xiii, Fe xii, Fe xi, Fe x, Fe viii, O v, and He ii. The
hottest line, Fe xv, shows the fastest upflow velocity and the second-highest line, Fe xiv, shows thesecond-highest upflow velocity (130 km s−1 ). The upflow velocities of other Fe lines also follow theorder of temperature. All velocities are below the sound speed, but the dependence of velocities ontemperature is similar to the dependence of sound speed on temperature. To complement the global
dynamics to EIS data, we use EIT data. In this talk, we discuss the characteristics of the plasma
which shows the blue shift in the plage region.

21

Discovery of Small-Scale Horizontal Magnetic Structures in the Photosphere
R. Ishikawa1 , S. Tsuneta1,2 , H. Isobe3 , Y. Suematsu2 , K. Ichimoto2 , S. Nagata4 , Y. Katsukawa2 ,T. Shimizu5 , B.W. Lites6 , R.A. Shine7 , T.D. Tarbell7 , and A.M. Title7(1) Department of Astronomy, University of Tokyo(2) National Astronomical Observatory of Japan(3) Department of Earth and Planetary Science, University of Tokyo(4) Kwasan and Hida Observatories, Kyoto University(5) Institute of Space and Astronautical Science, JAXA
(6) High Altitude Observatory, NCAR
(7) Lockheed-Martin Solar and Astrophysics Laboratory
We discover two different types of episodes (hereafter referred to as type 1 and type 2) on the appearance of strong horizontal magnetic fields with solar optical telescope aboard Hinode. Type 1 is an
emergence of strong thin horizontal magnetic fields associated with separating vertical components on
both ends. Its size is a few granules. We also detect strong area asymmetry of the Stokes V profile
about 8 minutes before the first emergence. One of the footpoints has very strong downflows (several
km s−1 ), while the region with strong linear polarization signal has small blue shift, indicating an
upward-moving horizontal flux. Type 2 appears to be more ubiquitous. Strong linear polarization
signals appear inside granules (not in inter-granules). Their size is smaller than granules, and lifetime
is longer than several minutes. We cannot see the significant vertical magnetic components at theedges of the horizontal magnetic fields region. We find that horizontal magnetic fields for the type 1
emergence is larger than that for type 2, and interpret that type 2 is more subject to the convective
motion due to its magnetic fields smaller than the equipartition field strength. We will summarize thenature of the two types, and discuss their origin.

22

Magnetoconvection, Chromospheric Reconnection and Coronal Heating: Implicationfrom MHD Simulation
H. Isobe
Department of Earth and Planetary Science, University of Tokyo
Observations by Hinode provides unprecedented oppotunity to study the magneto-convection dynamics and its conseqnece in the upper atmosphere. In this paper we present the results of magnetohydrodynamic simulations of convection-zone – corona coupling, as well as some preliminary analyses of
Hinode observations. The simulation setup is as follows: the domain includes the upper convection
zone, photosphere, chromosphere and corona. Convection is driven by radiative cooling in the photoshere, which is treated by the Newton approximation. When convection is developed and reached toa quasi-steady state, a vertical magnetic field is imposed. We have run the simulation with various
field strength.
As is well known, magnetic field is concentrated in the intergranular lanes. Moreover, we found that,when the imposed magnetic field is weaker than the equi-partition value with the kinetic energy of theconvection flows (about 400 G), the magnetic field in the convection zone becomes highly turbulent
and intermittent. As a consequence, fairly strong (400 G) horizontal magnetic field transiently appears
in the photosphere, at the top of the granular cells. These horizontal field undergoes reconnection
with the pre-existing “canopy” field in the chromosphere, and generates high-frequency Alfvén waves
and jets (spicules). Generation of high-frequency Alfvén waves is of particular interest because they
may have significant contributions to coronal heating and solar wind acceleration. Such transient
emergence of granular-scale horizontal field has been found in the data taken by the spectropolarimeterof Solar Optical Telescope. Preliminary analyses of the data and proposal of further observation will
be presented.

23

Takeo Kosugi and Indo-Japan Collaboration in Solar Physics
R. JainPhysical Research Laboratory, Ahmedabad
The great Japanese solar astronomer Takeo Kosugi was indeed a true friend of India. He took initiative to begin collaborative scientific efforts between Japan and India in order to exchange the solar
observing technology and to carry out investigations on the energetics and dynamics of solar flaresin context to Solar X-ray Spectrometer (SOXS), Indian mission, and proposed Solar-B Japanese mission as well as ground-based optical and radio waveband observations through ISAS and PRL. We
present a few reminiscences of our collaboration. Next, we present the results of our joint investigations based on multi-wavelength study of a very impulsive solar flare of 10 March 2001, observed by
Yohkoh mission in simultaneous to optical observations made in India, and SOXS flare observations
from India and simultaneous observations from ground based facilities in Japan. The 10 March 2001
flare was well covered with many space based and ground based observatories viz. Yohkoh, SOHO,WAVES/WIND, Nobeyama, and Hiraiso, Japan. The observations revealed that the flare was very
impulsive with a very hard X-ray spectrum and γ-rays suggested that non-thermal emission was mostdominant. On the other hand an unusual phenomenon of association of CME with highly impulsive
flare was observed. We conclude from SOHO/MDI and Mitaka magnetograms that the energy buildup took place due to photospheric reconnection/ flux cancellation, and further emergence of positive
flux increased the shear > 80◦ at the flare location, which seems the main cause for the trigging of theflare. The flare showed two bright compact sources in H-alpha. We co-aligned the Hα, SXR, HXR,
MW and magnetogram images within the instrumental limit. The flare showed single HXR source,which is found spatially associated with one of the Hα kernels. We report the unusual feature of therotation of HXR and Hα sources during the impulsive phase of the flare. From the spatial correlationof multi-wavelength images of the different sources, we conclude that this flare has a three-legged
structure. We briefly discuss the X-ray and optical emission characteristics of microflares observed by
SOXS in 4 – 25 keV in simultaneous to Hα observations made at NAOJ, and explores the possibilityof their candidature to heat the solar corona.

24Plasma Properties of Penumbral Fine Structures
J. Jurcak1 , S. Tsuneta1 , Y. Suematsu1 , K. Ichimoto1 , T. Shimizu2 , Y. Katsukawa1 , S. Nagata3 ,B.W. Lites4 , R.A. Shine5 , T.D. Tarbell5 , and A.M. Title5(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Kwasan and Hida Observatories, Kyoto University(4) High Altitude Observatory, NCAR
(5) Lockheed-Martin Solar and Astrophysics Laboratory
We present a set of sunspot observations obtained with the Hinode spectropolarimeter at various
positions on the disk. We are analyzing the limb-side parts of the penumbra using a one-component
inversion technique. This choice is motivated by the high angular resolution of 0.300 attained by theobservations. The dependence of the resulting stratifications on the position on the disc is analyzed
and discussed. The retrieved stratifications of plasma parameters are compared with those predictedby current models of penumbral fine structure.

25

Velocity Structure of Jets in Coronal Holes
S. Kamio1 , H. Hara1 , T. Watanabe1 , K. Matsuzaki2 , S. Imada1 , A. Asai1 , and Hinode EIS Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
Doppler velocity of jets in coronal holes was studied with the Extreme-ultraviolet Imaging Spectrometer (EIS) on board Hinode. The EIS is capable of obtaining EUV spectra and context images in two
wavelength ranges, 17 – 21 nm and 25 – 29 nm. Its high resolution and efficiency are suitable forstudying fine structures of the corona and the transition region.
An analysis of Doppler shifts in a coronal line (Fe xii) has indicated that loop-shaped bright points
are red-shifted. Faint elongated jets above the bright points are blue-shifted by 30 km s−1 . The
corresponding velocity features are not detected in transition region lines. It suggests that the observed
jets are high-velocity flow with a coronal temperature. These characteristics are found in many brightpoints in coronal holes. On the other hand, bright points outside coronal holes do not indicate
significant velocity.
Bright points in coronal holes can be explained as the line-of-sight velocity component of the reconnection jets, which are caused by magnetic flux emergence in pre-existing open fields. A smaller
velocity associated with the bright points outside coronal holes implies difference in magnetic fieldstructures in the corona.

26

Derivation of dBz /dz from Stokes Profiles and its Application to
Azimuth Ambiguity Resolution
S. Kamio1 , K. Ichimoto1 , M. Kubo2 , S. Tsuneta1 , Y. Suematsu1 , Y. Katsukawa1 , T. Shimizu2 ,S. Nagata3 , and Hinode SOT Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Kwasan and Hida Observatories, Kyoto University
We derived the longitudinal gradient of magnetic field strength (dBz /dz) from Stokes profiles by using
Artificial Neural Networks (ANN) and used it for resolving the azimuth angle ambiguity of magnetic
field with a simple algorithm. ANN can infer physical quantities from Stokes profiles with an exceptionally high speed compared to ordinary inversion codes. Carroll and Staude (2001) and Socas-Navarro(2005) demonstrated that ANN can obtain vector magnetic field components and Doppler velocities.
We constructed an ANN to derive the sign of the dBz /dz component from Stokes profiles by training
it with a synthesized data set of 16000 profiles. Its evaluation with synthesized profiles indicates thatthree-layer ANN can determine the sign of dBz /dz with 90 % accuracy, though simpler two-layer
ANN failed to achieve that. High quality Stokes profiles obtained with the Spectro-Polarimeter (SP)on board Hinode were processed with the ANN.
Once the sign of dBz /dz is determined from Stokes profiles, gradients of horizontal components
can be estimated from the equation div B = 0. We compare the results with that of potential field
extrapolation method and discuss the advantages and disadvantages of this method.

27

Micro-Flares Observed with Hinode/XRT
R. Kano1 , T. Sakao2 , and XRT-Team(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
Micro-flares are tiny events, but the coordinated observation between photospheric magnetic fields
and coronal activities for micro-flares will reveal the elementary processes of coronal heating. The
X-Ray Telescope (XRT) on the Hinode satellite has many advantages for micro-flare observations.
The first is its high spatial resolution (1 arcsec/pixel), of course. However, we would like to pointout the flexibility of its exposure cadence. If we accept to restrict the observation duration, XRT canobserve active regions in cadence as high as 3 s.
We used such high-cadence observation data for NOAA 10923 taken on November 14, 2006. Nine
micro-flares occurred in 30 minutes. We found that the time variation of their intensities is more
impulsive than Yohkoh/SXT observed. The duration of each impulsive peak is about 30 s. Someof the events accompanied jet structures. We will show magnetic features below the micro-flares,
observed by the Hinode/SOT.

28

Chromospheric Micro-Jets Discovered above Sunspot Penumbrae
Y. Katsukawa1 , S. Tsuneta1 , Y. Suematsu1 , K. Ichimoto1 , T. Shimizu2 , M. Kubo2 , S. Nagata3 ,T.E. Berger4 , T.D. Tarbell4 , R.A. Shine4 , and Hinode/SOT Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Kwasan and Hida Observatories, Kyoto University(4) Lockheed-Martin Solar and Astrophysics Laboratory
The Solar Optical Telescope (SOT) aboard Hinode allows us to observe dynamical activities in thephotosphere and the chromosphere with high and stable image quality of 0.2 arcseconds. This superior performance of SOT provides new findings of fine-scale transient activities occurring in thechromosphere. In this paper, we report the discovery of fine-scale jet-like phenomena ubiquitously
observed above sunspot penumbrae. The jets are identified in image sequences of a sunspot taken
through a Ca ii H line filter at 3968 Å. Their length is typically between 3000 and 10000 km, and theirwidth is smaller than 500 km. It is notable that their lifetime is shorter than 1 minute. Those small
spatial and temporal scale possibly makes it difficult to identify the phenomena in existing groundbased observations. The jets are easily identified when a sunspot is located far from the disk center,and motion of the bright features suggests that mass is erupted from the lower chromosphere to theupper atmosphere. Velocities of the motion are estimated to be 50 to 100 km s−1 from their lateralmotion of intensity patterns. The velocities are much faster than sound speeds in the chromosphere.
A possible cause of such high-speed jets is magnetic reconnection at the lower chromosphere resulted
from un-combed magnetic configuration in penumbrae which is suggested by vector magnetic fieldmeasurements in the photosphere.

29Formation Process of a Light Bridge Observed with Hinode/SOT
Y. Katsukawa1 , T. Yokoyama2 , T.E. Berger3 , S. Tsuneta1 , Y. Suematsu1 , K. Ichimoto1 ,T. Shimizu4 , M. Kubo4 , S. Nagata5 , and Hinode/SOT Team
(1) National Astronomical Observatory of Japan(2) Department of Earth and Planetary Science, University of Tokyo(3) Lockheed-Martin Solar and Astrophysics Laboratory(4) Institute of Space and Astronautical Science, JAXA
(5) Kwasan and Hida Observatories, Kyoto University
The formation of a light bridge is important in understanding the process of break-up of a sunspot.
SOT on Hinode successfully observed evolution of a light bridge forming in the middle of a spot in
AR 10923 from 12 to 17 November 2006. This observations was the first time ever for us to see theevolution of a light bridge longer than several days with high spatial resolution. Signatures of its
formation was the intrusion of penumbral filaments into an umbra before the light bridge appeared.
When the formation of the light bridge started, many umbral dots were observed emerging around theleading edge of penumbral filaments, and rushing into the umbra along a trail. Their inward velocities
were about 1.5 km s−1 which were significantly faster than the velocities of penumbral intrusion, 0.7
km s−1 . The light bridge is found to be the consequence of continual emergence and inward motionof the umbral dots. This observation clearly indicates close relationship among penumbrae, umbral
dots, and light bridges. The Spectro-Polarimeter (SP) in SOT provided physical conditions in thephotosphere around the light bridge and the umbral dots rushing into the umbra. We found that themagnetic field strength was about 1 kG weaker than the surroundings in the light bridge and in theumbral dots, and the upflow velocities of about 0.5 km s−1 were associated. This suggests that there
is a hot gas with weak field strength penetrating from the deep sub-photospheric layers to near thevisible surface, and the inward motion of the umbral dots is not the motion of magnetic field lines,
but the motion of the hot gas pushing through the surrounding magnetic fields.

30

Cooperative Observation of Umbral Dots between Hinode/SOT and
Domeless Solar Telescope at Hida
R. Kitai1 , H. Watanabe1 , S. Ueno1 , S. Nagata1 , K. Shibata1 , R. Muller2 , K. Ichimoto3 ,and Hinode SOT Team
(1) Kwasan and Hida Observatories, Kyoto University(2) Midi-Pyrénées Observatory, France(3) National Astronomical Observatory of Japan
Hinode SOT will give us high spatial resolution images of solar fine structure. We can follow andtrack temporal evolution of fine features in the photosphere without any fear of seeing distortionof the images. Umbral dots are small and faint features in dark umbral regions, so it has beena very difficult observational task thus far to get their basic properties and their characteristics oftemporal evolution. In this paper, we will propose to do cooperative observation between Hinode/SOT
imaging and Domeless Solar Telescope spectroscopic observations. The science target is to get thechracteristics of umbral dots, such as (1) temperature from two-color imaging, (2) magnetic filed
from spectropolarimeter, (3) Doppler velocity from spectroscopy, (4) identification of chromosphericcounterparts from Hα imaging, and (5) proper motions. The derived properties of umbral dots will
give us information on the convective energy flow in the umbral atmosphere and temporal evolutionof sunspots, especially on the decaying mode of spots.

31

X-ray Bright Points Observed with Hinode/XRT
J. Kotoku1 , R. Kano1 , T. Sakao2 , and Hinode XRT Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
X-ray bright points (XBPs) are small scale phenomena detected in soft X-rays everywhere in the quiet
Sun. Understanding of their characteristics is very important because they might contribute to therequired power to keep the corona at its high temperature. Although the physical processes in these
phenomena may turn out to be the same physical processes as in big flares, the truth has not yet been
known because of the difficulty in fabricating X-ray optics with high angular resolution compared toother wave lengths.
We observed XBPs with the X-Ray Telescope (XRT) aboard the Hinode satellite launched in
September 2006. XRT has high angular resolution (1 arcsec) and covers wide temperatures (ranging
from < 1 MK up to > 20 MK) ever achieved as a grazing-incidence imager for the Sun. The observed
fine images suggest that XBPs have not only a simple loop or a cusp structure but more complicatedmorphologies. We report those results of observations with Hinode XRT.

32

Formation of Moving Magnetic Features and Penumbral Magnetic Fields
with Hinode/SOT
M. Kubo1 , K. Ichimoto2 , T. Shimizu1 , S. Tsuneta2 , Y. Suematsu2 , Y. Katsukawa2 , S. Nagata3 ,Z.A. Frank4 , T.D. Tarbell4 , R.A. Shine4 , A.M. Title4 , B.W. Lites5 , and D.F. Elmore5(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of Japan(3) Kwasan and Hida Observatories, Kyoto University(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCAR
We investigate the formation process of Moving Magnetic Features (MMFs) observed with Hinode/SOT. Moving magnetic features are small magnetic elements moving outward in the moat region
surrounding mature sunspots. We derive vector magnetic fields of MMFs around simple sunspots
near the disk center. Most of MMFs whose polarity is opposite to the sunspot have large redshift
around the penumbral outer boundary. We find that some of them have Doppler velocities of about
10 km s−1 and such large Doppler motion is observed only in the Stokes V profile. The Stokes Q and
U profiles in the same pixel do not have any significant Doppler motions. Horizontal magnetic fieldsof the penumbra frequently extend to the moat region and the MMFs having horizontal fields with
their polarity being the same as the sunspot are formed. The MMFs whose polarity is opposite to thesunspot appear around the outer edge of the extending penumbral fields. We also found penumbral
spines, which have more vertical magnetic fields than the surroundings, branch off at their outer edge.
MMFs having relatively vertical fields with their polarity being the same as the sunspot are detachedfrom the outer edge of the branch. The branch of penumbral spine is formed where granular cells
appear in the penumbra.

33

Evolution of Vector Magnetic Fields in a Flare Productive Active Region
NOAA10930 with the Hinode/SOT
M. Kubo1 , T. Yokoyama2 , Y. Katsukawa3 , S. Tsuneta3 , Y. Suematsu3 , K. Ichimoto3 , T. Shimizu1 ,S. Nagata4 , T.D. Tarbell5 , R.A. Shine5 , A.M. Title5 , B.W. Lites6 , and D.F. Elmore6(1) Institute of Space and Astronautical Science, JAXA
(2) Department of Earth and Planetary Science, University of Tokyo(3) National Astronomical Observatory of Japan(4) Kwasan and Hida Observatories, Kyoto University(5) Lockheed-Martin Solar and Astrophysics Laboratory(6) High Altitude Observatory, NCAR
We successfully observed the evolution of vector magnetic fields in an active region NOAA10930
with Hinode/SOT for one week (2006/12/8-2006/12/15). A lot of flares including four X-class flares
occurred in this active region. It was very difficult to perform such continuous observation with ahigh spatial resolution and a constant measurement quality in the case of ground-based telescopes.
An evolving sunspot with positive polarity moved around an opposite polarity old sunspot in contact
with each other. Elongated magnetic structures with positive and negative polarities were alternately
located along the polarity inversion line (PIL) in between the two sunspots before the X3.4 class flare.
Such elongated magnetic structures were formed due to flux emergence around the following edge ofthe evolving sunspot, and then the PIL became very complicated. The flare ribbons were observedin Ca ii H with Hinode/SOT and they appeared at the PIL. One of the two flare ribbons evolved
along the PIL. After the X3.4 class flare, the PIL became smooth and a region with azimuth angle
perpendicular to their surroundings disappeared. And then the elongated magnetic structures withnegative polarity merged into the old sunspot with negative polarity and positive ones merged into
the evolving sunspot with positive polarity. These elongated magnetic structures with alternating
polarity disappeared during a day after the X3.4 class flare.
We will discuss photospheric magnetic activity responsible for large flares by using a time series ofhigh spatial resolution vector magnetic fields observed with Hinode/SOT.

34

Three-Dimensional Coronal Magnetic Field Analysis Based on Hinode/SOT
Vector Magnetograms
K. Kusano1 , S. Inoue2 , T. Yokoyama3 , S. Tsuneta4 , Y. Suematsu4 , K. Ichimoto4 , Y. Katsukawa4 ,T. Shimizu5 , S. Nagata6 , and SOT Team
(1) The Earth Simulator Center, JAMSTEC(2) Solar-Terrestrial Environment Laboratory, Nagoya University(3) Department of Earth and Planetary Science, University of Tokyo(4) National Astronomical Observatory of Japan(5) Institute of Space and Astronautical Science, JAXA
(6) Kwasan and Hida Observatories, Kyoto University
The understanding of three-dimensional magnetic field structure on solar coronal active regions is
crucially important to reveal the mechanism of solar activity, in particular the triggering mechanism of
solar flares. However, since only photospheric magnetic field is observable, three-dimensional magnetic
field in solar corona has to be reconstructed from photospheric magnetogram as a solution of boundaryvalue problem based on the force-free field approximation. For this purpose, Hinode/Solar Optical
Telescope (SOT) is an ideal tool, because of its high resolution and the quality of continuity. In
this paper, aiming to reveal the characteristic magnetic structure in the triggering region of solar
flares, we have analyzed three-dimensional magnetic field of active region NOAA 10930, using vector
magnetograms observed by Hinode/SOT Spectro-Polarimeter (SP). The extended magnetofrictional
code has been developed for this study by adopting the multi-grid relaxation technique and the
optimized searching procedure of initial trial function. The results indicated that magnetic field in
the region, where GOES X3.4 flare occurred on 13 Dec. 2006, 02:20 UT, consisted of multiple flux
systems of different magnetic shear. Furthermore, we have found that pre-flare brightening of Xshape, which was observed during a couple of hours prior to the onset of the flare, were located on
the site where magnetic vector sharply changes the azimuth. The results are basically consistent withthe so-called Reversed Shear Flare Model, which had predicted that solar flare should be triggeredby the nonlinear development of resistive tearing mode instability growing on magnetic shear reversal(Kusano et al. 2004 ApJ, and Kusano 2005 ApJ). The comparison analyses between flare kernels
observed by XRT and the three-dimensional field line structure was also performed.

35

Has Hinode Found the Missing Turbulent Magnetic Field of the Quiet Sun?
B.W. Lites1 , H. Socas-Navarro1 , Z.A. Frank2 , R.A. Shine2 , T.D. Tarbell2 , A.M. Title2 ,K. Ichimoto3 , S. Tsuneta3 , Y. Katsukawa3 , Y. Suematsu3 , M. Kubo4 , and T. Shimizu4(1) High Altitude Observatory, NCAR
(2) Lockheed-Martin Solar and Astrophysics Laboratory(3) National Astronomical Observatory of Japan(4) Institute of Space and Astronautical Science, JAXA
Measurements with the Hinode Spectro-Polarimeter (SP) of the quiet Sun allow characterization of
the weak, mixed-polarity magnetic flux at the highest angular resolution to date (0.300 ), and with goodpolarimetric sensitivity (0.025 % relative to the continuum). The image stabilization of the Hinodespacecraft allows long integrations with degradation of the image quality only by the evolution of
the solar granulation. From the Stokes V profile measurements we find an average solar “Apparent
Flux Density” of 14 Mx cm−2 , with significant Stokes V signals at every position on the disk at all
times. However, there are patches of meso-granular size (5 – 1500 ) where the flux is very weak. At
this high sensitivity, transverse fields produce measurable Stokes Q, U linear polarization signals overa majority of the area, with apparent transverse flux densities in the internetwork significantly larger
than the corresponding longitudinal flux densities. When viewed at the center of the solar disk, theStokes V signals (longitudinal fields) show a preference for occurrence in the intergranular lanes, andthe Q, U signals occur preferably over both granule interiors and lanes.

36A Multi-Wavelength View of an Active Region Structure around a Filament Channel
L.L. Lundquist1 , A.A. van Ballegooijen1 , K.K. Reeves1 , T. Sakao2 , E.E. DeLuca1 , and N, Narukage2(1) Smithsonian Astrophysical Observatory(2) Institute of Space and Astronautical Science, JAXAThe combination of multi-wavelength, high resolution, high cadence data from the Hinode X-Ray
Telescope (XRT) and the Transition Region And Coronal Explorer (TRACE) give an unprecedented
view of solar active region dynamics and coronal topology. We focus on examples of filament structures
observed by TRACE and XRT in December 2006 and February 2007. Co-alignment of observationsin these two instruments yields a striking picture of the coronal structures, with loops lying bothalong and above the filament. Overlying loops exhibit remarkable dynamics while the filament lies
dormant, and numerous X-point and triple-leg structures undergo repeated brightenings. We also
employ magnetic field data from SOLIS to compare a non-linear force-free model of the coronalmagnetic field with the observed loops.

37

Solar Flares Observed with Yohkoh/HXT
S. Masuda
Solar-Terrestrial Environment Laboratory, Nagoya University
Late professor Takeo Kosugi was a PI of the Hard X-ray Telescope (HXT) on board Yohkoh. Thanks
to his strong leadership and his enlightening strategy, HXT succeeded in detecting more than 3,000
solar flares during its ten-year operational period and revealed a lot of new features in solar flares.
This contributed much toward the realization of the RHESSI satellite. In this presentation, notablehighlights among many scientific results obtained from HXT observations are reviewed.

38

First Discovery of Ellerman Bombs by Hinode/SOT with Hida/DST
T. Matsumoto1 , R. Kitai1 , K. Shibata1 , S. Nagata1 , K. Otsuji1 , T. Nakamura1 , S. Tsuneta2 ,Y. Suematsu2 , K. Ichimoto2 , T. Shimizu3 , Y. Katsukawa2 , T.D. Tarbell4 , B.W. Lites5 , R.A. Shine4 ,and A.M. Title4(1) Kwasan and Hida Observatories, Kyoto University(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCARHigh resolution Ca ii H broad band filter images obtained by Solar Optical Telescope (SOT) aboard
Hinode reveals that there are many small scale (≈ 1 arcsec) bright points outside sunspots and inside
emerging flux regions. We identified some of these bright points with Ellerman bombs by using Hαimages taken by Domeless Solar Telescope at Hida observatory. The Ca bright points identified withEllerman Bombs are usually associated with bipolar magnetic field structures. Moreover, Ca ii H
images show a series of arch-like filaments with a size of ≈ 5 arcsec whose foot points correspond to
the locations of the Ca bright points. In this study, we will report the difference between Ellerman
bombs and other Ca bright points without Hα features.

39Classification of Phenomena Observed by EIS aboard HinodeK. Matsuzaki1 , H. Hara2 , T. Watanabe2 , A. Asai2 , S. Imada2 , S. Kamio2 , M. Shimojo2 ,K. Ichimoto2 , T. Sakao1 , N. Narukage1 , and US-UK EIS Team(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of JapanEUV Imaging Spectrometer (EIS) aboard Hinode observes plasma in temperature range of several 104
K to several 106 K by detection of multiple spectral lines emitted in the wavelength of 170Å–210Å
and 250Å–290Å. EIS can achieve observation with three times better spectral resolution (R ≈ 4000)
than previous EUV instruments and spatial resolution of 100 . In this talk, spectral analysis of typicalcorona and transition region observed by EIS will be demonstrated. Distribution of line intensities offeatures observed in maps will be discussed.

40

Hinode/XRT Observations of a Coronal Sigmoid
D.E. McKenzie and R.C. Canfield
Department of Physics, Montana State University
We present the first observations of an X-ray sigmoid made with the Hinode X-Ray Telescope,co-aligned with those of TRACE and SoHO/MDI. XRT’s extraordinary angular resolution (1 arcsec/pixel) and the sigmoid’s location near disk center combined to provide an unprecedented view ofthe formation and eruption of this phenomenon. XRT observed the sigmoid over a 23-hour periodwith a cadence of at least one image per 30 s, and with a much lower cadence for several days prior.
The first motions associated with eruption of the sigmoid started at 0600 UT on 12 February 2007;
the first brightening of the ensuing X-ray arcade was seen at 0740UT.
The images during the pre-eruptive phase, which ends with the onset of large-scale motions, show:+ The overall S-shape of the sigmoid is not defined by any single X-ray loop. Rather, many
individual loops collectively comprise an S-shaped pattern.
+ The S-shape is comprised of two separate J-shapes, whose straight sections lie anti-parallel to
one another in the middle of the S, on opposite sides of the magnetic polarity inversion line.
+ During the several-day span of the XRT observation, the S-shape gradually becomes better
defined.
The images during the eruptive phase show:+ Approximately 100 minutes before any soft X-ray flaring begins, a diffuse linear structure, almost
as long as the sigmoid, lifts off from the middle of the S. It shows slight clockwise rotation.
+ The X-ray flare begins with the appearance of a sheared arcade of short loops, in the area
centered between the two J-shaped patterns of the sigmoid.
+ Within 16 hours of the start of the flare, no S-shape remains.
Taken together, these features provide strong support for the Bald-Patch Separatrix Surface model ofsigmoids put forth by Titov and Demoulin (1999).

41

An Emerging Flux Region Observed with Hinode/SOT on 11 December 2006.
T. Miyagoshi1 , Y. Katsukawa2 , S. Tsuneta2 , Y. Suematsu2 , K. Ichimoto2 , T. Shimizu3 , S. Nagata4 ,and Japan and USA SOT Team
(1) The Earth Simulator Center, JAMSTEC(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Kwasan and Hida Observatories, Kyoto University
We have studied an emerging flux region observed by Hinode/SOT on 11 December 2006. As the flux
emerged, bright points often appeared and disappeared in both G-band and Ca ii filter observations.
Three patterns are found in the observations. The first is simultaneously observed bright points atthe same location in both (G-band and Ca ii) filter observations. The second is bright points observed
only with the Ca ii filter (not found in G-band at the same time and at the same location). The thirdis bright points observed only with the G-band filter (not found in Ca ii at the same time and at thesame location).
The size of this emerging flux region is about 15 000 km. On the other hand, the wavelength withthe largest growth rate in the Parker instability at the photosphere is about 4000 km. Therefore webelieve that two or three loops may have emerged side by side. Then they may have interacted witheach other and resulted in bright points. Dark lanes were also observed as the flux emerged. We haveinvestigated the relation of the observed dark lanes in G-band and Ca ii filters. We found that thedark lane in the Ca ii observation appeared later than in the G-band one.

42

Center-to-Limb Variation in Stokes Profiles of Magnetic Fluxtubes Observed with
Hinode Spectropolarimeter
S. Morinaga1 , T. Sakurai2 , S. Tsuneta2 , Y. Suematsu2 , K. Ichimoto2 , J. Jurcak2 , S. Nagata3 , andB.W. Lites4(1) Department of Astronomy, University of Tokyo(2) National Astronomical Observatory of Japan(3) Kwasan and Hida Observatories, Kyoto University(4) High Altitude Observatory, NCAR
It is very important to investigate the magnetic structure and evolution of pores, growing small
sunspots without penumbra, in order to understand the formation of sunspots. We here present
spectro-polarimetric measurements of several pores with the Solar Optical Telescope (SOT) aboard
Hinode with various viewing angles. We analyzed the Stokes V amplitude and area asymmetries andconfirmed that the asymmetries are depressed at the center of the pores while they show large positive
values in the surrounding area; this is consistent with the previous report by Leka and Steiner (2001).
In addition to this ring of positive asymmetry, we found another larger ring structure. The larger ringshows positive asymmetries at the disk-center side, whereas it shows negative asymmetries again at
the limb side. In this presentation, we suggest that the center-to-limb-variation of the magnitude of
the area asymmetry and its pattern indicate a systematic inflow into the pore from the surroundings.

43Performance of Image Stabilizer of Hinode Solar Optical Telescope
S. Nagata1 , S. Tsuneta2 , Y. Suematsu2 , K. Ichimoto2 , Y. Katsukawa2 , T. Shimizu3 , T.D. Tarbell4 ,B.W. Lites5 , R.A. Shine4 , and A.M. Title4(1) Kwasan and Hida Observatories, Kyoto University(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCAR
Solar Optical Telescope of Hinode has an image stabilizer system. The system consists of a tip-tilt
mirror in the Optical Telescope Assembly (OTA) and a correlation tracker in the Focal Plane Package(FPP). The digital servo loop is operated at 580 Hz, and its designed crossover frequency is about 20
Hz. The system performance was investigated during the initial operation period, and the pointing
was found to be stabilized about 0.01 arcsec for 10 s period. The stability of the pointing achieved
with the image stabilizer enables the polarimetirc observations with high signal to noise ratio.

44

Dynamical Properties of Flux Tubes and its Relationship to Convective Collapse
Revealed by Spectropolarimeter of Hinode/SOTS. Nagata1 , S. Tsuneta2 , Y. Suematsu2 , K. Ichimoto2 , Y. Katsukawa2 , T. Shimizu3 , T.D. Tarbell4 ,B.W. Lites5 , R.A. Shine4 , A.M. Title4 , L.R. Bellot Rubio6 , and D. Orozco Suárez6(1) Kwasan and Hida Observatories, Kyoto University(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCAR
(6) Instituto de Astrofı́sica de Andalucı́a, Granada
We present the dynamical properties of photospheric fluxtubes observed with Spectro Polarimeter ofSolar Optical Telescope (SOT) aboard Hinode. Based on the high time cadence observations withsmall FOV of 4 × 40 arcsec at disk center quiet sun, we found the merge of flux in the inter-granularlanes, and formation of bright point in the continuum. At the bright point, very strong red shift with
about 6 km s−1 was observed. During the formation of bright point, the Stokes V -profile amplitude
and its separation increased. We discuss the formation of kilo Gauss fluxtube formation based on theobservations.

45

Coronal Temperature Diagnostics with Hinode X-ray Telescope
N. Narukage1 , T. Sakao1 , R. Kano2 , M. Shimojo2 , S. Tsuneta2 , T. Kosugi1 , E.E. Deluca3 ,L. Golub3 , M. Weber3 , J.W. Cirtain3 , and Japan-US XRT Team(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of Japan(3) Smithsonian Astrophysical Observatory
An X-ray telescope (XRT) on board the Hinode satellite observes the Sun in X-rays with high special
resolution (1 arcsec ≈ 730 km on solar the disk). This telescope has nine X-ray filters with different
temperature responses. Using these filters, the XRT can detect the coronal plasma with a wide
temperature range from less than 1 MK to more than 10 MK. Moreover, based on observations withmore than two filters, we can estimate the coronal temperature. In this paper, we use the filter ratio
method for coronal temperature diagnostics. Using this method, we can easily estimate the averaged
temperature of the coronal plasma along the line-of-sight. This method has been used frequently
in the past, but the high quality XRT data give us temperature maps with unprecedented accuracy
and resolution. The XRT usually takes the full Sun images with two kinds of filters four times aday. Using this data and filter ratio method, we can obtain full Sun temperature maps with highspecial resolution. In our analysis, we can derive reliable temperatures not only in active regions but
also in quiet regions and coronal holes. This map can be created with the data set of one synoptic
observation. This means that we can obtain four maps a day. The result is a full Sun temperature
movie that gives us an unprecedented view of the time evolution of solar temperature. In this meeting,
we will show the full Sun temperature movie and our coronal temperature analysis results.

46

X-ray Waves Observed with Hinode X-ray Telescope
N. Narukage1 , T. Sakao1 , R. Kano2 , H. Hara2 , A. Asai2 , S. Tsuneta2 , T. Kosugi1 , E.E. Deluca3 ,L. Golub3 , Japan-US XRT Team, and Japan-UK EIS Team(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of Japan(3) Smithsonian Astrophysical Observatory
When solar flares occur, wave-like disturbances and shock waves are sometimes observed in several
kinds of wavelengths. In 1960, the coronal shock wave was indirectly detected in Hα, i.e., the intersections of the coronal shock waves and chromosphere are observed as the H-alpha wave-like disturbances
called “Moreton waves”. In 2000’s, the soft X-ray telescope (SXT) on board Yohkoh discovered several
wavelike disturbances (shock waves) in the solar corona associated with flares, which we call “X-ray
waves”. The shock waves are very faint phenomena and propagate at a high speed (little faster thanthe Alfvén velocity ≈ 1,000 km s−1 ). So, it is difficult to observe them. An X-ray telescope (XRT)
on board Hinode was expected to detect such faint shock waves, because of its high spatial-resolution
and high S/N. On 13 December 2006, the XRT detected the wavelike disturbance associated with
an X-class flare. The speed of the wavelike disturbance is about 630 km s−1 . In this flare, a typeII radio burst, which shows the existence of a shock wave, was also observed with the Hiraiso Radio
Spectrograph (HiRAS). Moreover, EUV Imaging Spectrometer (EIS) on board Hinode scanned theregion where the X-ray wavelike disturbance was propagated. We analyzed these data and examine
whether the wavelike disturbance is shock wave or not. In this meeting, we will show the analysis
results.

47

Discovery of Cool Cloud-Like Structures in the Corona with Hinode/SOT
T.J. Okamoto1,2 , S. Tsuneta2 , Y. Katsukawa2 , K. Ichimoto2 , Y. Suematsu2 , T. Shimizu3 ,S. Nagata1 , K. Shibata1 , T.D. Tarbell4 , R.A. Shine4 , T.E. Berger4 , B.W. Lites5 , and D.C. Myers6(1) Kwasan and Hida Observatories, Kyoto University(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCAR
(6) NASA/Goddard Space Flight Center
We observed an active region AR10921 near the west limb of the solar disk on 9 November 2006 with a
Ca ii broadband filter of Hinode/SOT. In addition to spectacular spicules, we found a large cloud-likestructure located 10 000 – 20 000 km above the limb. The cloud had a very complex fine structure withdominant horizontal thread-like structure. Some features were moving horizontally and also showed
clear vertical oscillatory motions. The periods and amplitudes of these oscillations were 130 – 250 s
and 200 – 850 km, respectively. The vertical oscillatory motion sometimes had a coherence length aslong as 16 000 km. We conclude from various observational features that this vertical oscillation isa signature of Alfvén waves propagating along the horizontal magnetic fields. We will discuss their
origin and implications.

48

Hinode/SOT High Resolution Observation of Small Scale Magnetic Flux
Emerging around a Sunspot
K. Otsuji1 , K. Shibata1 , R. Kitai1 , S. Nagata1 , T. Matsumoto1 , T. Nakamura1 , S. Tsuneta2 ,Y. Suematsu2 , K. Ichimoto2 , T. Shimizu3 , Y. Katsukawa2 , T.D. Tarbell4 , B.W. Lites5 , R.A. Shine4 ,and A.M. Title4(1) Kwasan and Hida Observatories, Kyoto University(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCAR
We studied small-scale emerging flux regions outside of a sunspot penumbra with Hinode/SOT in the
Ca ii H line, G-band, and Fe 6302 Å magnetograms. We found that they have the following properties.
1. In the initial phase of flux emergence, these emerging flux regions are observed as filaments in the
Ca ii H line and as dark granular lanes in the G-band, respectively. The width of Ca filaments isabout 200 (≈ 1500 km) and wider then that of granular lanes, which is 100 (≈ 700 km). The life timeof the Ca filaments is about 20 minutes. It is not clear yet whether the granular lanes appear before
the formation of the Ca filaments.
2. Ca bright points are seen at the footpoints of Ca filaments. G-band bright points are also observedat the same positions. These bright points correspond to the areas of strong magnetic fields. Initially,
the distance between the two footpoints of a Ca filament is ≈ 200 . The growth speed of the filamentsis ≈ 4 km s−1 at the initial stage then it decreases to ≈ 1 km s−1 .

49

Many Faces of the Fine Structure of the Eclipse Corona
V. Rušin1 , M. Druckmüller2 , M. Minarovjech1 , and M. Saniga1(1) Astronomical Institute, Slovak Academy of Sciences(2) Institute of Mathematics, Brno Technical University, Czech Republic
The inner white-light corona (up to 2 solar radii) can only be observed during total solar eclipses. New
mathematical methods of the corona image processing and digital photo cameras or CCD cameras
allow us to detect very faint structures (of a few arcsec) in this part of the corona, even from images
taken with relatively small telescopes (1–2 m in the focal length). In the present paper we will
discuss such structures as observed during the last few solar eclipses, mainly those of 2002, 2005
and 2006. Obtained results show that the white-light corona is highly structured not only in thesense of a variety of different types of its classical “objects”, e.g., polar plumes, helmet streamers,
threadlike streamers, etc, but also within these objects themselves. Voids, loops, radial and nonradial threads, and other yet-undefined dark structures (“empty space”?) are well visible especiallyinside helmet streamers. This strongly indicates that the classical picture of the corona characterized
by a hydrostatic distribution of density and temperature is no longer a viable assumption, and it israther magnetic forces that play a dominant role in shaping and structuring this part the corona.
Given a remarkable similarity between the EUV corona as observed by SOHO and the white-lightcorona observed by us during the above-mentioned eclipses up to two solar radii, it is suggestive formodeling to approximate the “missing” observations of the white-light corona by those of the EUV
one. Moreover, the last eclipse observations also indicate that the peaks of some prominences extend
well into the white-light corona. So, the next total eclipses of the Sun, of 1 August 2008 and 22 July
2009, offer an excellent opportunity for preparing joint observations from Hinode and ground-based
eclipse teams.

50

A New View of the Solar Corona with the X-Ray Telescope (XRT) aboard HinodeT. Sakao1 , E.E. DeLuca2 , R. Kano3 , S. Tsuneta3 , H. Hara3 , K. Matsuzaki1 , M. Shimojo3 ,K. Shibasaki3 , T. Kosugi1 , I. Nakatani1 , and the Japan-US XRT Team1,2,3,4(1) Institute of Space and Astronautical Science, JAXA
(2) Smithsonian Astrophysical Observatory(3) National Astronomical Observatory of Japan(4) NASA/Marshall Space Flight Center
We present pieces of initial results made with the X-Ray Telescope aboard the Hinode satellite launchedin September 2006. The XRT is a successor of the Soft X-ray Telescope (SXT) for Yohkoh, andemploys Walter-I-like grazing incidence optics. Thanks to the increased effective area (larger mirror)
as compared to the SXT with significant effort on high-precision polishment for the mirror surface, the
XRT images the corona with the highest angular resolution (1 arcsec) ever achieved with solar X-ray
telescopes while maintaining exposure times (i.e., cadence) similar to those with SXT. Furthermore,
due to the use of a back-thinned CCD device coupled with an optimized set of focal-plane analysis
filters, the XRT is capable of imaging coronal plasmas in a wide and continuous temperature range
from 1 MK to above 10 MK.
Since the beginning of its observation in late October 2006, the XRT has been continuously taking
images of the X-ray Sun at a rate exceeding 1000 images a day. The XRT has so far revealed many
new aspects of coronal phenomena which include (1) transient brightening activities (microflares) inactive regions, (2) temperature structure of the corona, (3) frequent X-ray jets in polar regions, (4)flares, and so on. Introductory overview on the XRT observations will be given together with scientificsignificance of the XRT.

51

Observations of Solar Flares with Hinode XRT
T. Sakao1 , K. Ichimoto2 , R. Kano2 , M. Kubo1 , E.E. DeLuca3 , K. Shibasaki2 , T. Minoshima4 ,Japan-US XRT/SOT Team1,2,3,5 , and Suzaku-HXD Team(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of Japan(3) Smithsonian Astrophysical Observatory(4) Department of Earth and Planetary Science, University of Tokyo(5) High Altitude Observatory, NCAR
(6) NASA/Marshall Space Flight Center
Soft-X-ray imaging observations of the corona prior to the onset, and in the early phase of, solar
flares are expected to provide us with key clues to understand magnetic field structure which leads
to explosive energy release and subsequent particle acceleration that take place in flares. The X-Ray
Telescope (XRT) aboard the Hinode mission is equipped with a unique capability in that it can image
detailed structure of high-temperature (> 2 MK) coronal loops with the highest angular resolution (1arcsec) ever achieved as a solar X-ray telescope.
We report XRT observations of X-class flares that commenced in December 2006 in NOAA AR10930,
with emphasis on the X3.4 flare on December 13. The soft X-ray flare in this event was initiated instrongly-sheared bundles of fine loops along a magnetic neutral line about 10 minutes before the onsetof the impulsive phase (identified by hard X-rays and microwaves with the HXD-WAM instrument
aboard Suzaku satellite and Nobeyama Radio Polarimeter, respectively). Evolution of the flaring loop
systems in the early phase of the flare towards the onset of the impulsive phase will be presented
and their timing relationship with explosive energy release as indicated by impulsive emission of hard
X-rays and microwaves discussed.

52

Initial Analysis of Hinode/SOT Helioseismology Data
T. Sekii1 , A.G. Kosovichev2 , S. Tsuneta1 , and SOT Team
(1) National Astronomical Observatory of Japan(2) HEPL, Stanford University
We present initial analysis of various helioseismology data acquired by Hinode/SOT. Hinode/SOT
provides opportunity for studying solar wavefield in high resolution. One big goal would be to study
active regions using tomographics means, but the data can also be used to investigate wave generationand propagation in turbulent magnetized plasma, including sunspot oscillations and flare-induced
waves. We report on some initial analysis of G-band and H-line intensity oscillations.

53

Kosugi-san and Nobeyama Solar Radio Observatory
K. Shibasaki
Nobeyama Solar Radio Observatory, NAOJ
Kosugi-san started his science career at Nobeyama Solar Radio Observatory as a post graduate studentof University of Tokyo in 1972. From the beginning, he had been interested in particle acceleration
process in solar flares and his life-long research was devoted to this problem. He started in thefield of metric wavelength, then moved to microwave which is more directly related to high energy
particles produced in solar flares. He also was interested in hard X-ray emission from accelerated
particles. Yohkoh and Nobeyama Radioheliograph were realized almost simultaneously due to his
great contribution. Still, we do not understand the particle acceleration mechanism in solar flares.
With Hinode and Nobeyama Radioheliograph, we wish to solve this problem in near future and toreport to Kosugi-san the answer.

54

Ca ii H Anemone Jets Discovered outside Sunspots Observed with Hinode/SOT
K. Shibata1 , T. Nakamura1 , T. Matsumoto1 , K. Otsuji1 , S. Nagata1 , R. Kitai1 , Hinode/SOT Team,and Hida Observatory Team
(1) Kwasan and Hida Observatories, Kyoto University
Solar Optical Telescope (SOT) aboard Hinode discovered tiny jets in the chromosphere outside
sunspots with Ca ii H broad band filter. The widths of the jets are less than 0.3 arcsec (i.e., < 200km), and their velocities are 5 – 20 km s−1 . The life time of jets are a few minutes. The smallbright points (or nanoflares) appeared near the footpoints of the jets. The shape of the jets and brightpoints is similar to those of the anemone jets observed with Yohkoh/SXT and Hinode/XRT. It is likelythat these tiny Ca jets are small scale version of anemone jet, suggesting that these are produced bymagnetic reconnection between small bipole (tiny emerging flux ?) and pre-existing (locally uniform)
magnetic field.

55

Spatial Distribution of Stokes-V Area-Asymmetries with Hinode/SOT
K. Shimada1 , S. Tsuneta1,2 , J. Jarcak2 , Y. Suematsu2 , K. Ichimoto2 , T. Shimizu3 , Y. Katsukawa2 ,S. Nagata4 , B.W. Lites5 , R.A. Shine6 , T.D. Tarbell6 , and A.M. Title6(1) Department of Astronomy, University of Tokyo(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Kwasan and Hida Observatories, Kyoto University(5) High Altitude Observatory, NCAR
(6) Lockheed-Martin Solar and Astrophysics Laboratory
Rich information such as line-of-sight velocity gradient is extracted from Stokes-V profiles. We performed a simple investigation on the high-resolution spatial distribution of the normalized Stokes-V
area-asymmetries. Stokes-V asymmetry maps show fine filamentary structure in penumbra. MilneEddington analysis indicates that such filaments have more horizontal, weaker magnetic fields withoutward flow. Inner ends of such filaments are brighter in the continuum, and have higher temperature.
This suggests anti (diamagnetic) flux tubes with outward cooling plasma flow. In addition to the wellknown penumbral asymmetries, there are islands (one to a few arcsec) with higher area-asymmetry
scattered in the moat region and neutrals sheet. Overview of these regions will be presented.

56

Calibration for Co-Alignment among Images from the Three Telescopes of Hinodewith Sub-Arcsecond Accuracy:
Mercury Transit, DC Offset, and Orbital Variations of Telescope Pointing
T. Shimizu1 , R. Kano2 , H. Hara2 , Y. Katsukawa2 , K. Ichimoto2 , S. Tsuneta2 , Y. Suematsu2 ,E.E. DeLuca3 , L.L. Lundquist3 , R.A. Shine4 , T.D. Tarbell4 , N. Narukage1 , T. Sakao1 ,and the Hinode Team(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of Japan(3) Smithsonian Astrophysical Observatory(4) Lockheed-Martin Solar and Astrophysics Laboratory
Understanding of magnetic coupling from the photosphere to the corona is one of observational goals
to be archived by the Hinode mission. Studies using coordinated data from three telescopes on
Hinode are expected to provide major improvement in our understanding of heating and dynamics
in the solar atmospheres. For such observational studies, precise spatial alignment of images fromthe three telescopes is required. Our goal is to establish co-alignment procedure with accuracy inorder of 0.5 arcsec or better. This presentation will give an introduction of Hinode between-telescopes
image co-alignment method and then discuss the latest status of calibration works for establishing theco-alignment procedure. For active region observations with sunspots, sunspots are used as fiducial
to co-align XRT data on SOT data. Coronal and chromospheric features can be used for EIS vs
XRT and EIS vs SOT, respectively. Satellite jitter in order of 1 arcsec or less is included withorbital variation of pointing in the series of XRT and EIS data, whereas image stabilization system(correlation tracker) removes the satellite jitter and orbital variation from the series of SOT images.
The telescopes pointing is moved to track the region of interest in case of tracking mode. Telescope
pointing show orbital variation in order of a few arcsec, which can be well predicted from Hinode orbit
information. For SOT vs XRT, it is confirmed that orbital variation is well predicted with sub-arcsec
accuracy. Using Mercury transit observed on November 8, 2006, the roll orientation of images fromeach telescope as well as the DC offset of pointing among the telescopes have been well determined.
Modeling co-alignment is under development and it is the only method for quiet Sun observations.

57

Magnetic High-Speed Local Flows Revealed in Hinode Optical Stokes Observations
T. Shimizu1 . K. Ichimoto2 , Y. Katsukawa2 , Y. Suematsu2 , S. Tsuneta2 , S. Nagata3 , R.A. Shine4 ,T.D. Tarbell4 , B.W. Lites5 , and US-Japan SOT Team(1) Institute of Space and Astronautical Science, JAXA
(2) National Astronomical Observatory of Japan(3) Kwasan and Hida Observatories, Kyoto University(4) Lockheed-Martin Solar and Astrophysics Laboratory(5) High Altitude Observatory, NCAR
The SOT spectro-polarimeter has, for the first time, been providing Stokes profiles of magnetic sensitive lines with 0.3 arcsec spatial resolution and 0.1 % photometric accuracy under seeing free condition.
When we examine SOT Stokes profiles, we can easily recognize that remarkable Stokes V profiles withenhanced signal at the red wing side exist at various locations on the solar surface. The Stokes V
profiles with enhancement on the red wing suggests that high speed downward flows with speed exceeding the sound velocity are formed in vertical oriented magnetic fields. The authors have foundthree types of such high-speed flows in umbra, penumbra, in moat region around sunspots, and alsoin quiet regions. The authors will discuss the nature of these flows.

58

Fine Structures of Solar X-ray Jets
M. Shimojo1 , N. Narukage2 , R. Kano1 , T. Sakao2 , S. Tsuneta1 , J.W. Cirtain3 , L.L. Lundquist3 ,E.E. Deluca3 , and L. Golub3(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Smithsonian Astrophysical Observatory
The X-ray telescope (XRT) aboard Hinode satellite has the great spatial/time resolution in X-ray
range. And, the observations using XRT have revealed the fine structures of solar corona. From theobservations, we found the fine thread structures in the X-ray jets and the structures move dynamicallylike wave. We also found that some X-ray jets start just after small loop expansion in the footpoint
brightening. The observation results suggest that the reconnection process X-ray jets is very similar
to that in large flares.

59

In-Orbit Optical Performance of Hinode/SOT in G-band (430 nm) Estimated with a
Phase Diversity Method
Y. Suematsu1 , K. Ichimoto1 , Y. Katsukawa1 , S. Tsuneta1 , T. Shimizu2 , and SOT Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXAThe Solar Optical Telescope (SOT) carried by Hinode was designed to perform a high-precision polarimetric observation of the Sun in visible light spectra with a spatial resolution of 0.2 – 0.3 arcsec.
The SOT is a sophisticated instrument and consists of two separate optical parts; the Optical Telescope Assembly (OTA) which is 50 cm aperture Gregorian telescope feeding the light into following
observing instruments which is called the focal plane package (FPP) made of two filtergraphs anda spectro-polarimeter. The performance of the OTA is important because a spatial resolution andits temporal stability is mainly determined by this component. The image of sub-arcsecond G-band(430.5 nm) bright points clearly indicates that the SOT achieves the diffraction-limit on orbit. We
have studied the on-orbit optical performance of SOT using a phase diversity method. In this paper,
we describe the method and result of the phase diversity and discuss on-orbit performance of the SOT.

60

High Resolution Observation of Spicules with Ca ii H Filtergraph of Hinode/SOT
Y. Suematsu1 , K. Ichimoto1 , Y. Katsukawa1 , S. Tsuneta1 , T. Shimizu2 , T. Okamoto1,3 , S. Nagata3 ,and SOT Team
(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Kwasan and Hida Observatories, Kyoto University
High cadence observation with a Ca ii H broadband filtergraph (passband of 0.25 nm) of the Solar
Optical Telescope (SOT) aboard Hinode has revealed dynamical nature of limb spicules. Thanks
to a diffraction-limited and low-scattered light property of the instrument, we can track the detailed
evolution of individual spicules for the first time with a spatial resolution of 0.2 arcsec. The spicules in
Ca ii H are typically several arcsec tall and have multi-thread structure; each threads are a few tenthof arcsec wide. It should be stressed that most spicules do not show a simple up-and-down motion
along a rigid path line. They start with bright structure emanating from Ca ii H bright region, getwiden and diffused with time and ascent, showing expansion with lateral or even helical motion in tall
events. Small and short lived spicules tend to fade out after ascent. We will present new findings of
spicule dynamics in different magnetic environments and discuss about long standing controversy ofits motion and evolution.

61

Ubiquitous Alfvén Waves in the Chromosphere
T.D. Tarbell1 , B. De Pontieu1 , S.W. McIntosh2 , V.H. Hansteen3 , M. Carlsson3 , C.J. Schrijver1 ,A.M. Title1 , and SOT Team
(1) Lockheed-Martin Solar and Astrophysics Laboratory(2) Southwest Research Institute, Boulder(3) Institute of Theoretical Astrophysics, University of OsloWe see direct evidence of Alfvén waves in the middle to upper chromosphere as imaged in Ca ii
3968 Å timeseries with Hinode/SOT. Our observations focus on spicules at the limb, and straw-likefeatures associated with network and plage on the disk. The high spatial and temporal resolution of
Hinode/SOT allows us to directly observe how these jet-like features undergo significant transverse
motions (0.5–1 Mm) that are driven by Alfvén waves with strong amplitudes of 20–30 km s−1 andperiods of 150–500 s. Preliminary estimates of the energy flux carried by these waves strongly suggeststhat they may play a significant role in the energy balance of the upper atmosphere, especially forthe solar wind and quiet Sun corona. We study the generation and propagation of these waves bycomparing our Hinode observations with advanced 3D radiative MHD simulations that encompass theconvection zone up through the corona.

62

Rapid Changes in the Small Scale Magnetic Fields and the Chromosphere
A.M. Title
Lockheed-Martin Solar and Astrophysics Laboratory
FPP magnetograms show examples of magnetic field evolution on the spatial and temporal scale of
granulation. Individual features can appear and disappear on the time scale of 120 s. In Ca ii H post
flare cooling loops have structures at or near the diffraction limit of the telescope. The transverse
velocity of the loops is on the order of 30 km s−1 and the repeat pattern in on the order of 10 s. Thissuggest that the pattern of loops is moving transversely. Surges at the limb are observed to repeat
with a time separation of 30 to 40 s. The vertical velocity of the individual fronts is about 50 km s−1
initially slowing to 30 km s−1 10 arcsec above their base. The transverse velocity of the events is 10– 15 km s−1 .

63High-Sensitivity Observations of Quiet-Sun Magnetic Fields by Using both
Extreme-Limb and Sun-Center Spectro-Polarimetric Data
S. Tsuneta1 , Y. Suematsu1 , K. Ichimoto1 , T. Shimizu2 , Y. Katsukawa1 , S. Nagata3 , B.W. Lites4 ,D. Orozco Suárez5 , R.A. Shine6 , T.D. Tarbell6 , and A.M. Title6(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Kwasan and Hida Observatories, Kyoto University(4) High Altitude Observatory, NCAR
(5) Instituto de Astrofı́sica de Andalucı́a, Granada(6) Lockheed-Martin Solar and Astrophysics Laboratory
Stokes V is much more sensitive to magnetic fields than Stokes Q and U , and extreme (80◦ or beyond)limb should be observed with Hinode spectro-polarimeter to reveal the static and dynamic propertiesof vector magnetic fields of the quiet Sun. (80◦ from sun center corresponds to 100 – 150 km above
the nominal height.) We employ wide-FOV snapshot data as well as high-cadence small-FOV data forthe north and south poles, east and west limb (all with similar equatorial distance from the center)as well as sun center for this purpose. Strong vertical fields are highly packed in the inter-granularlanes located in the sun-center, while in the limb region ubiquitous isolated Stokes V (i.e. fields
horizontal to local surface) patches are seen. Larger (1–2 arcsec) magnetic patches seen in the poles
show unipolar-Q with bipolar U and V . This suggests ice-cream-cone-like structure. There appears
to be more such magnetic islands in the poles than in the equatorial limb (quiet Sun).

64

Attempt to Detect Alfvén Waves with SOT aboard Hinode
S. Tsuneta1 , Y. Suematsu1 , K. Ichimoto1 , T. Shimizu2 , Y. Katsukawa1 , S. Nagata3 ,D. Orozco Suárez4 , B.W. Lites5 , R.A. Shine6 , T.D. Tarbell6 , and A.M. Title6(1) National Astronomical Observatory of Japan(2) Institute of Space and Astronautical Science, JAXA
(3) Kwasan and Hida Observatories, Kyoto University(4) Instituto de Astrofı́sica de Andalucı́a, Granada(5) High Altitude Observatory, NCAR
(6) Lockheed-Martin Solar and Astrophysics Laboratory
Flux tube on the sun may carry linear and torsional Alfvén waves generated by photospheric motion.
Photospheric motion of 2 km s−1 would provide magnetic fluctuation of 40 G for 1 kG tube with the
Alfvén speed of 50 km s−1 . This may be close to the detection limit of the Stokes Q and U signals
for flux tubes located in the sun center. However, for flux tubes located near the limb, the fluctuation
would be seen in the Stokes V signal, and can be detectable. We also may be able to confirm the 90
degree phase shift between magnetic fluctuation and velocity fluctuation, which is easier to observe forflux tubes near the limb. Detection of waves with its spectra would be important in terms of coronalheating and solar wind acceleration. An attempt to detect waves along flux tubes will be reported.

65

On the Moat-Penumbra Relation
S. Vargas-Dominguez1 , J.A. Bonet1 , V. Martinez Pillet2 , Y. Katsukawa3 , Y. Kitakoshi4 , and
L. Rouppe Van der Voort4,5(1) Instituto de Astrofı́sica de Canarias, Tenerife(2) National Astronomical Observatory of Japan(3) Department of Astronomy, University of Tokyo(4) Institute of Theoretical Astrophysics, University of Oslo
(5) Center of Mathematics for Applications, University of Oslo
Granular proper motions in solar active regions (AR) have been studied by using local correlation
tracking techniques. Time series of high-resolution images are used to compute the horizontal flows
for every AR. Large-scale radial outflows, the well-known sunspots moats, have been detected aroundthe spots in all the AR. However, these outflows are only found in those umbral core sides without
penumbra. These results evidence a relation between the moat flow and the penumbrae. Hinode will
give us the opportunity to get into the details of this relation and establish the precise link we suggest
between the moat and the well-known Evershed flow.

66Evolution of Vector Magnetic Fields in Canceling Magnetic Features
J. Wang , C. Jin, M. Zhao, G. Zhou, and J. Zhang
National Astronomical Observatories, Chinese Academy of Sciences
Magnetic flux cancellation was first described by Livi, Wang, Martin (1985) and Martin, Livi, Wang
(1985) as the mutual flux disappearance in closely-spaced magnetic flux of opposite polarity. The twocanceling components of opposite polarity were referred to as a canceling magnetic feature (Wang etal. 1988). Flux cancellation has been found to associate with most (if not all) types of magnetic activity, such as flares, filament eruptions, initiation of coronal mass ejections, and ubiquitous small-scale
activity on the quiet Sun. Suggestions of the role of flux cancellation in chromospheric and coronalheating were also suggested by various authors (Sturrock et al. 1999; Longcope and Kankelborg 1999;
von Rekowski et al. 2006). Therefore to diagnose the physical process underline the observed flux
cancellation will lead to better understanding on the origin of solar activity. So far controversial
interpretations, e.g., flux submergence (Parker 1987), flux emergence of U-loops (Spruit, van Ballegooijen, and Title 1987), magnetic reconnection in the lower solar atmosphere (Wang and Shi 1993),
reconnection-submergence (Priest et al. 1994), flux emergence of O-loops (Lites et al. 1995) were
proposed by different authors.
We propose observation campaigns on the nature of flux cancellation by observing the vector fieldevolution in canceling magnetic features. Three types of target regions are suggested to choose:(1) small- to middle-size active regions (ARs), (2) periphery of big ARs, and (3) quiet Sun region
with either enhanced or quiet network. As flux cancellation and new emerging flux are intrinsicallyassociated, the regions with newly emerging flux regions are of priority in the selection. The accurate
vector magnetograms will require observations from the Spectro-polarimeter at the line-pair of Fe i
630.15 and 630.25 nm; The knowledge of the life-story of flux evolution will ask the observations fromthe Narrowband Filter Imager at the same Fe i line-pair for photosphere and the Mg b i 517.27 nm
for chromosphere; The knowledge of temperature and dynamic structures will need the observations
from Broadband Filter Imager from Ca ii line, CH line and lines for temperature measurements. The
average rate of flux cancellation in ARs is of the magnitude 1018−19 Mx/hour and on the quiet Sun,
1018 Mx/hour; while the total flux involved in an AR and an area of network field is in the orders ofmagnitude of 1021−22 Mx and 1020 Mx, respectively. Therefore for AR observations, 3–5 day durationof the observations is necessary when the AR located close to the central meridian; to the quiet Sun
observations 2–3 day duration would be necessary. We would require the kind collaborations fromthe colleagues in SOT team to get training and knowledge in magnetic calibration and data analysis.
The response of transition region and corona to the observed flux cancellation in the photosphereis extremely important to learn the physics of flux cancellation. We would ask the coordinative
observations form EIS and X-ray telescope to study the coupling of flux cancellation and the heatingof higher atmosphere.

67

Temperature and Density Structures of the Solar Corona— A Test of Diagnostic Capability of the EIS Instrument on board Hinode —T. Watanabe1 , H. Hara1 , J.L. Culhane2 , L.K. Harra2 , G.A. Doschek3 , J.T. Mariska3 , P.R. Young4 ,and the Hinode EIS Team
(1) National Astronomical Observatory of Japan(2) Mullard Space Science Laboratory(3) Naval Research Laboratory(4) Rutherford Appleton Laboratory
Increased diagnostic capability of the EIS instrument on board Hinode is tested with a set of ironemission lines located in the two EIS observing wavelengths (170 – 210 Å and 250 – 290 Å). First-light
spectra of a small active region show iron emission lines at the ionization stages of Fe viii (185.2 Å
and 186.6 Å) through Fe xvii (204.7 Å, 254.9 Å, and 269.4 Å), showing emission measure distribution
at upper transition-region, low and high coronal temperatures. Decay phase spectra of a C-class flareconfirms the presence of Fe xvii at 254.9 Å, as well as those lines of flare temperatures; Fe xxiv (192.0
Å and 255.1 Å) and Fe xxiii (263.8 Å) reveal that the emission measure distribution extends above
107 K.

68

Milne-Eddington Model Fitting Program of the Hinode/SOT-SP Data
T. Yokoyama1 , Y. Katsukawa2 , M. Shimojo2 , S. Tsuneta2 , Y. Suematsu2 , K. Ichimoto2 , T. Shimizu3 ,M. Kubo3 , S. Nagata4 , B.W. Lites5 , H. Socas-Navarro5 , and the Hinode Japan-USA SOT Team(1) Department of Earth and Planetary Science, University of Tokyo(2) National Astronomical Observatory of Japan(3) Institute of Space and Astronautical Science, JAXA
(4) Kwasan and Hida Observatories, Kyoto University(5) High Altitude Observatory, NCAR
The Hinode SOT/SP obtains line polarization profiles of magnetically sensitive Fe lines. By fittingthese profiles under a given atmospheric model, we can measure the detailed magnetic and dynamic
structure of the photosphere. We will report the status of the development of the fitting program andthe initial results obtained by using it. This code is based on the Milne-Eddington model and is anextended version of the MELANIE and PIKAIA originally maintained by the HAO group in USA.

69

Study of Non-Potential Magnetic Field Inferred from
Photospheric Vector Magnetograms and Soft X-ray Images
H. Zhang
National Astronomical Observatories, Chinese Academy of Sciences
The measurements of photospheric vector magnetic field and soft X-ray images provide some basic
information on the development and relaxation of non-potential magnetic flux and the relationshipwith the solar eruptions. The following projects are proposed in the study of Hinode data:(1) The formation of non-potential magnetic field and helicity in solar active regions inferred from thevector magnetograms and soft X-ray images.
(2) The large-scale topology of magnetic field inferred from local and full-disk photospheric vector
magnetograms and soft X-ray images.
(3) The comparison between the vector magnetograms from Hinode and ground-base observations.

70