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1/8AAPPS Bulletin June 2009, Vol. 19, No. 3 11

Hinode "A New Solar Observatory in Space"


Saku Tsuneta

Hinode Science Center, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan

1. MAGNETIC FIELD AND COS-

MOS

It is a remarkable and fascinating fact thata solitary star like the Sun emits intenseX-rays from its outer atmosphere. Obser-vations with Japan-US Yohkoh satellite[1] show that all the sporadic heating frommajor ares to ubiquitous tiny bursts in

the solar corona is due to magnetic recon-nection; a process to efciently annihilate

magnetic elds with opposite direction

into heat, jets and non-thermal accelera-tion. Magnetic eld does dissipate in the

corona with time scale 1012

faster than thatof the classical Ohmic dissipation. Thoughthis leads to an attractive conjecture thatthe solar corona in general is heated byensemble of tiny bursts ([2, 3] and refer-ences therein), precise mechanism for the

heating of solar corona and accelerationmechanism of solar wind is, however,unknown.

These activities on the surface of thestar are driven by magnetic eld created

by interaction of ow and elds below the

photosphere (dynamo mechanism). Themagnetic eld strength on the surface of

the sun exceeds 1 kG, while that at the bot-tom of the convection zone may reach 100

kG. They are too strong, far stronger thanthe equi-partition magnetic eld strength,whose energy is the same as that of the lo-cal convection motion. Though a dynamomechanism can amplify field strengthupto the equi-partition eld strength, it

is perceived not possible to have eld

strength beyond the threshold. Such

too-strong magnetic eld can be found

elsewhere in the universe, namely puls-ers (10

12G), magneters (10

15G), galaxies

and clusters of galaxies (a few micro G),which is again too strong in terms of thatin early universe (10

-17G, [4]). Dynamo

mechanism for the sun and these objectsis poorly understood.

2. HINODE SPACECRAFT

The Hinode spacecraft ([5], see Fig. 1),previously known as Solar-B, was success-fully launched in September 2006 from theUchinoura Space Center in Japan using aJAXAs M-V launch vehicle. On 25 Octo-ber 2006, it started its scientic operation.

Its orbit is a sun-synchronous orbit thatprovides 9-month continuous observa-tions. It comprises an observatory style

set of instruments that function togetherto answer the fundamental question ofhow magnetic elds are formed and how

they dissipate to create the solar corona.This subsequently addresses all phenom-ena that have an impact on the Sun-Earthsystem, such as the formation of the solarwinds (both slow and fast), triggering ofares with intense non-thermal particle

acceleration and coronal mass ejections,

formation and maintenance of laments

and prominences.

The concept of Hinode is that two X-rayand EUV telescopes observe the dissipa-tion part of the magnetic life-cycle history,while the visible light telescope observes

generation and transport of magnetic eldsimultaneously. Hinode is the Japansthird solar mission with participation ofNASA and UK STFC (then PPARC).Observations of Sun from space in Japanstarted with Hinotori satellite as early as1981. Hinotori took the hard X-ray imagesof solar ares above 20 keV for the rst

time. This is followed by highly successfulYohkoh mission, which carries both hard

Fig. 1: Image of the Hinode spacecraft in orbit.

Saku Tsuneta

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2/812 AAPPS Bulletin June 2009, Vol. 19, No. 3

Research Activities on Astronomy and Astrophysics in Japan

and soft X-ray telescopes. The Hinodemission is designed based on Yohkoh re-sults and recent progress in ground-basedastronomy. This review summarizes howthe new results from Hinode are address-ing these critical questions as well asprobing fundamental physical processesthat will have applications in many otherscenarios across the universe.

There are three instruments onboard Hi-node, the Solar Optical Telescope (SOT),the X-ray Telescope (XRT), and the EUVImaging Spectrometer (EIS), each measur-ing critical parts of the suns atmospherefrom the surface (photosphere) to thechromosphere, the transition region andnally the outer and hottest part of the

atmosphere, the corona.

2.1. The Solar Optical Telescope (SOT)

SOT is the rst large optical telescope

own in space to observe the sun [6]. It

has an aperture of 50 cm and achieves anangular resolution of 0.25" (175 km on thesun) covering a wavelength range from380-650 nm. It consists of 2 components,the Optical Telescope Assembly (OTA:[7]) and the Focal Plane Package (FPP).The FPP includes the narrow-band (NFI)and the wide-band (BFI) ltergraphs and

the Stokes spectropolarimeter (SP). Thiscomplex instrument allows measurementsof the magnetic eld both in the longitu-dinal and transverse directions, Dopplershifts, and imaging in the range fromthe low photosphere through to the chro-

mosphere very accurately under precisecalibration [8].

2.2. The X-ray Telescope (XRT)

XRT is an advanced solar X-ray telescope[9, 10] with the highest angular resolu-tion of 1". It is a Wolter Type I grazing

incidence telescope that uses 2 reections

to focus soft X-rays onto a CCD array. Itcan provide both full sun and partial diskimages. Filters ranging in thickness by afactor of 10,000 provide a huge dynamicrange able to measure very weak featuresin coronal holes and very large ares. The

temperature range extends from 1 mil-lion K to 30 million K. This temperaturerange is much wider than that of the softX-ray/EUV Telescopes on board Yohkoh,SOHO and TRACE.

2.3. The EUV Imaging Spectrometer

(EIS)

EIS is an imaging spectrometer [11] builtby a consortium consisting of UCL-MSSL,RAL, NRL, GSFC, UiO, and NAOJ. EISwas designed to probe the dynamics of thesolar atmosphere with a spatial resolutionof 1". It uses two EUV wave-bands whichwere chosen to measure plasma withtemperatures ranging from 50,000 K to20 million K. EIS is a exible instrument

with the ability to measure high-resolu-tion spectra along with imaging achievingvelocity resolutions of several km/s, andit can also observe fast cadence (seconds)monochromatic images. The two wave-bands cover a total of 90 containing at

least 500 spectral lines of which 55% areidentied to come from previously known

atomic transitions [12].

3. A NEW OBSERVATIONS ON

SOLAR MAGNETIC FIELD

Magnetic field carries energy throughwaves and fluctuation, and can storeenergy. It dissipates stored energy withmagnetic reconnection, and induces MHDinstability and eruptions. Another aspectof magnetic field is that it suppressescross-eld transport for mass and heat, and

suppress convection i.e. energy transport.In the following sections, highlights of thenew results from Hinode during its initialoperational phase are introduced.

Fig. 2 shows images of the sunspot andthe suns surface captured by the opticaltelescope. The sizes of the sunspot rangefrom between several thousand kilometersto several tens of thousands of kilometers.By enlarging the suns image further,structures called granules can be seen, asshown in Fig. 2, in which bubbling gasesow in swirls of convection over an area

measuring about 1,000 km. Small whitespots seen between the granules corre-spond to strong magnetic elds. It is still a

mystery how these structures were formed,but thanks to Hinode, it has become pos-sible to observe these changing featuresfor the first time. Fig. 3 shows a sideview of the sun with a sunspot positionedalong the edge. Bright emissions appearfrequently around the sunspot, and mate-

Fig. 2: Sunspot on the suns surface captured by the optical telescope onboard Hinode. The observations were made at a wavelength of460 nm. (The colors in the image have been articially enhanced and differ from the actual colors.) Convection called granules can beseen in the photosphere (right). Small spots between the convection cells are magnetic elements (the minimum unit of a magnetic eld)that have an exceptionally strong magnetic eld. (Courtesy of NAOJ, JAXA, and NASA.)

50,000 km size of the earth

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rial jets up like a fountain to an altitudeof 20,000 km.

Hinode shows magnetic eld structures

in a new light, and two major discoveriesbeing made by Hinode are reported here.

3.1. Super Equi-Partition Field

The photospheric magnetic ux tubes with

kG eld strength and spatial scale of a few

100 km are ubiquitously found across theentire solar surface. Those ux tubes ap-pear as small bright points in Fig. 1. Theeld strength should have been limited by

the equi-partition magnetic energy (typi-cally 400 G) corresponding to the kineticenergy density of the granular ows. Thus,

further intensication is necessary to ex-plain the kG eld strength ux tubes. A

theory was that the plasma in ux tubes

emerged from below cools and falls dueto suppression of heat, and the ux tube

narrows until the magnetic pressure ofthe evacuated ux tube balances with the

surrounding gas pressure. This processreferred to as convective collapse hasbeen studied for almost 30 years, and isnally conrmed with Hinode [13]. We

nd a good coincidence between the eld

strength intensification and the down-ward motion. The initial eld strength

of 400 G is intensied up to 2,000 G as

the downow grows to 6 km s1

in 150 s.Convective collapse ubiquitously takesplace in the convective atmosphere, andis an essential ingredient for formation ofux tube with intense magnetic eld.

3.2. Horizontal Magnetic Field and Lo-

cal Dynamo Process

The surface of the Sun is essentiallycovered with concentrated (< 1) verticalmagnetic ux tubes with eld strengths

of kG as shown above. This paradigm ischallenged by Hinode: Hinode discov-ered transient horizontal magnetic elds[Fig. 4], which are characterized by hori-zontal eld with random direction, size as

small as convection cell, life time as shortas convection turnover time, magneticeld strength smaller than equi-partition

strength. These unique properties arecompletely different from those of thevertical magnetic elements. The horizon-tal elds are ubiquitous, regardless of the

quiet sun or active regions, and their totalmagnetic ux is larger than that of verti-cal elds. It appears that convection layer

has an inherent property to produce suchhorizontal elds. We call this local dynamo

process ([14] and references therein). Itis totally unknown at this point how thisnew dynamo process and its resultant hori-zontal elds are related to global dynamo

process, which produces sunspots.

4. DYNAMIC X-RAY CORONA

While the optical telescope observes the

photosphere/chromosphere, the X-raytelescope captures images of the coronaand the high-temperature ares that range

from between several million and severaltens of millions of degrees. The sun viewedthrough the X-ray [Fig. 5] is completelydifferent from that seen in the visible light

range. The area around the sunspot, wherethe strong magnetic elds exist, is referred

to as an active region, from which X-raysfurther radiate. Many stripes can be seenaround the active region, which representthe magnetic lines of force that spreadupward from the photosphere.

There is now the possibility that the re-

sults of the observations of Hinode may beused to solve the coronal heating problem.Hinode has revealed there are strong verti-cal and horizontalmagnetic elds outside

sunspots, and strong coronal activity evenin areas without the sunspot. Sourcesof X-rays are scattered here and thereon the photosphere, and it still remainsa mystery as to how they were formed.Hinode expects to understand the solarcorona heating mechanism by comparingsuch information with information on themagnetic elds obtained by the optical

telescope. The current hypothesis is thateither nano-ares and/or some form of

Fig. 3: Dynamic solar activities around the sunspot as seen through the opticaltelescope; substances of temperatures of several tens of thousands of degreesare being sprayed into the solar atmosphere. (Courtesy of NAOJ, JAXA, andNASA.)

Fig. 4: (upper panel) granule (convection)pattern in white light. (lower panel) transienthorizontal magnetic eld. Bright while colorcorresponds to eld strength of 200 G or be-yond. (Courtesy of R. Ishikawa of NAOJ.)

16,000 km

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magneto-hydrodynamic waves propagat-ing open eld lines are responsible for the

heating of corona.

EIS has the capability of obtainingphysical information of the coronalplasma, such as temperature, density, andvelocity. An interesting discovery withEIS is the high-speed upows at footpoints

of coronal loops in active regions [15]and weakly emitting outows at the edge

of active regions in open magnetic eld

congurations [16, 17], both of which

have upflow velocities exceeding 100km/s. Interestingly, broad EUV emissionlines are found in these upow regions,

suggesting the presence of unresolvedne-scale dynamic structures that reects

how heating energy is deposited. EIS hasalso revealed that a typical coronal ll-ing factor in active region loops is about10% from its density diagnostic capability[18], which determines the electron den-sity of various structures in the transitionregion and corona with unprecedentedstatistics.

5. PROMINENCE, SPICULE AND

WAVES

The activity on the sun is known to bedriven by the magnetic fields that areprevalent everywhere. Hinode has higher

temporal, spatial and velocity resolutionthan any satellite previously and is probingwavelength regimes that have never hadsuch continuous time coverage available.This has allowed us to measure waves inthe atmosphere in a way we have beenunable to do before. In 1947 Alfvn pre-dicted the existence of magnetic wavescaused by the constant movement due toconvection on the surface of the sun. Theconvection disturbs the magnetic elds

causing waves and may then be dampedin the corona providing an energy sourcethat may create enough heating for theatmosphere and energy to accelerate thesolar wind. Attempts to measure Alfvnwaves have been ambiguous in previousground-based observations, but Hinodenow appears to be opening the door tothese waves being observed in many dif-ferent circumstances.

A spectacular example is solar promi-nences. These are large-scale, cool struc-tures that lie surrounded by the hot corona.It has been suggested that these are causedby plasmas maintained in coronal hori-zontal magnetic eld-line congurations.

Observations show horizontal threads ofplasma which have oscillatory behaviorwith periods around 170 s. This is consis-tent with Alfvn wave propagation which

may possibly heat the surrounding corona[19]. What comes as a surprise is that

prominences in the quiet Sun show darkupward ows that are turbulent and move

at speeds of 20 km/s [20]. The existence ofthese ows is a real challenge to the cur-rent MHD understanding of prominencesas they are inconsistent with the magneticsustainment of heavy low-temperatureplasma against gravity.

The chromosphere is highly structuredas can be seen in Fig. 2. At the solar limb,spiky features known as spicules are seenin abundance. Now with Hinode, observa-tions can be made continuously withoutbeing concerned about seeing condi-tions as is the case with ground-basedtelescopes. De Pontieu et al. (2007) [21]have analyzed these spicules and foundthat there are two types. The rst type

is formed when global oscillations andconvective ows leak into the atmosphere

causing shocks. These have timescales ofminutes and show persistent upward anddownward motions. The type II spicules(named straws) have lifetimes of seconds,are much thinner and move plasma atspeeds of over 100 km/s. These seem to berelated directly to the magnetic reconnec-tion process. Both types of spicules showa swaying behavior strongly indicative

Fig. 5: X-ray images of the entire solar surface pho-tographed by the X-ray telescope onboard Hinode.A punctuate structure called an X-ray bright pointwas identied for the rst time, which revealed thatthe corona is made up of magnetic loops. (Courtesyof NAOJ, JAXA, and NASA.)

Fig. 6: The right hand side shows a full sun XRT image with the box showing the EISFOV. The left EIS image is the intensity and the right image is the Doppler velocity.The blue arrow shows the source of the strongest outow. (i.e., [25], [17].)

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of Alfvn waves. They show amplitudesand periods that are consistent with the p-mode 5 min oscillation [22], and they haveenough energy to power the solar wind.

Jets of collimated, hot plasma have beenobserved for many years on the sun. Thesecan occur in the active region loops thatlie above sunspot groups or even withinthe coronal holes. One explanation ofthe formation of jets involves a scenarioin which emerging ux from below the

surface reconnects with coronal holes.Hinode now has the ability (thanks to itshigher spatial resolution) to observe jetsin signicantly more detail to study basic

physical processes [23]. Jets in coronalholes have been observed to have speedsof 200 km/s. However, a new componentthat occurs at the beginning of the jet for-mation has been discovered, high speed,reaching 800 km/s, close to the Alfvnspeed in the corona [24]. The characteris-tics of these jets are consistent with plasmabeing ejected at the Alfvn speed, whichis a direct observation of the outow jet

from the reconnection site. These smalljets may carry as much as a tenth of themass necessary for the solar wind.

These observations clearly show thatAlfvn wave or magneto-hydrodynamicswaves are ubiquitous in chromosphere andin corona, and this opens up a new researcheld to understand its role in the heating

and acceleration of coronal plasma, and todiagnose the Sun from below photospherethrough corona with seismic approach.

6. SOLAR WIND AND POLAR

REGION

The sun supplies a huge amount of plasmainto interplanetary space as solar wind. Itis well known that the solar wind consistsof two components, a fast solar wind thatcomes from predominantly coronal holesthat have open magnetic elds, and a slow

solar wind that comes from other openmagnetic elds, such as the boundary of

large-scale coronal holes and small-scalecoronal holes even though its source hasbeen debated for many years. Alfvnwaves as mentioned above are also criti-

cal for solar wind acceleration. However,in this paper we focus on the source ofsolar wind.

The slow solar wind has fluctuatingspeeds between 200-500 km/s. XRT hasobserved persistent and steady ows di-rectly at the edges of active regions [25]with speeds of over 100 km/s that persistfor days. The mass loss rate was estimatedto be 25% of the slow solar wind. UsingEIS alongside this dataset, the real Dopplerows can be then observed. Fig. 6 shows

the XRT image for context alongside theEIS data. The EIS data show the intensityof the corona on the left-hand side. Nowfor the rst time, the Doppler velocities can

also be observed (on the right hand sideof Fig. 6). The region of weakest emissionat the top of the active region shows thestrongest velocities [17]. Probing the mag-netic eld shows that this region is highly

extended, most likely open elds caused

by reconnection with a much smaller ac-tive region to the west of the one studied.These large-scale reconnections may beof signicant importance when aiming to

understand the slow solar wind.

We have also new observations related to

a fast solar wind. Tsuneta et al. (2008) [26]reported SOT observations of the magneticlandscape of the polar region of the sunwith an extremely high spatial resolutionand high polarimetric precision. Using aMilne-Eddington inversion, it was foundthat many vertically oriented magnetic ux

tubes with eld strengths as strong as 1

kG were scattered in latitude between 70and 90 [Fig. 7]. They all have the samepolarity, consistent with the global polarityof the polar region. The eld vectors have

been observed to diverge from the centersof the ux elements, consistent with a view

of magnetic elds that are expanding and

fanning out with height. The polar regionhas also been found to have ubiquitoushorizontal elds. The polar regions are

the source of the fast solar wind, which ischanneled along unipolar coronal magneticelds whose photospheric source is evi-dently rooted in the strong-eld, vertical

patches of ux. We conjecture that vertical

ux tubes with large expansion around the

photospheric-coronal boundary serve asefcient chimneys for Alfvn waves that

accelerate the solar wind.

Fig. 7: South polar view of the magnetic eld strength taken at 12:02:19-14:55:48UT on 16 March 2007. The original observing eld of view is 327.52'' (east-west)by 163.84'' (north-south) and was converted to a map seen from above the southpole. East is to the left, west is to the right, and the observation was carried outfrom the top down. Spatial resolution is lost near the extreme limb (i.e., near thebottom of the gure). The eld of view for the line-of-sight direction (163.84'')expands to 472.96'' as a result of correction for foreshortening. The pixel sizeis 0.16''. Latitudinal lines for 85, 80, 75, and 70 are shown as large circles,while the plus sign marks the south pole. The magnetic eld strength is obtainedfor pixels meeting a given threshold. (after [26].)

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7. GIGANTIC SOLAR FLARE:

13 NOVEMBER 2006 EVENT

Also observed on the surface of the sunare explosive phenomena called solarares that last for several minutes to sev-

eral hours and the eruption of substancesreferred to as high-speed jets caused bythe explosions. A magnetic eld controls

the activities in the corona, and largeexplosions take place frequently near thesunspot where magnetic eld lines have

complex structure.

Although the sun is now at the minimumof its activity level, we are still occasion-ally treated to an active region which pro-

duces solar ares. Such a region appearedin December 2006 just after the Hinodescientic operation started. Days before

the large X-are on 13 December 2006, the

active region had been monitored. Therewas a large negative polarity sunspot,and to the south of it emerged a smallerpositive polarity sunspot. Over the days ofthis evolution, the smaller sunspot rotateddramatically, colliding into the pre-existingsunspot [27]. The impact on the coronaabove of this shearing motion could beseen [28]. Just as the smaller sunspot wasemerging, the coronal loops were lyingperpendicular to the inversion line (mark-ing out the separation between positive andnegative polarity). At this stage the loopswere essentially potential with little storedenergy. By 12 December 2006, the storywas completely different. At this stage thenew sunspot had been emerging and rotat-ing at the surface, dragging the eld lines

around, and causing the magnetic loopsto become so sheared that they were nowlying parallel to the inversion line. A fewhours after this, a huge X-class are took

place there. Fig. 8 shows an image of agigantic are captured by Hinode, which

stretches to several tens of thousands ofkilometers. Even more dynamic video pic-tures captured by Hinode can be viewed onthe website of the National AstronomicalObservatory of Japan (NAOJ) at http://hi-node.nao.ac.jp/index_e.shtml.

During this X-class are, we measured

directly for the rst time what part of the

atmosphere erupted away from the sun.Imada et al. (2007) [29] analyzed the areon 13 December 2006 and found that thestrongest outows were away from the

main are site. The force of the are had

ripped off some of the plasma from thesun. Interestingly, there seems to be astrong relationship between this outow

and the temperature of the plasma. Thestrongest outows are from the hottest

plasma which provides a constraint to themechanism that forms this fast componentto the solar wind. Speeds of 1,000 km/swere measured at ACE from this event.

The sun is in a period of minimum activ-ity at the time of writing. Solar ares will

start to occur more frequently as the sunheads toward its period of maximum activ-ity around 2013-2014, when it will thenundergo a transformation that will makeit appear as a different star. Hinode is sureto change fundamentally the academicperspectives on solar observation throughthe analysis of clear and high-resolutionimages and spectroscopic data during theperiod of maximum activity.

8. MAGNETIC UNIVERSE

Recently, there is growing interest onthe role and behavior of magnetic eld

in the universe. Topics include X-rayares in proto-stars, galactic prominence

and spicule [30], X-ray ridge emissionnear Galactic center, jets from accretiondisks, non-thermal particle accelerationin clusters of galaxies, gamma-ray bursts,pulsers, and magnetors, relationship be-

tween magnetic eld in early universe and

galactic dynamo. As we saw here in thisbrief report, with rapid progress in spaceobservations, we are able to observe andresolve fascinating magneto-hydrodynam-ics phenomena occurring on the Sun. Sunis, needless to say, a natural laboratoryto be accessible through telescopes. In-deed, direct comparison with numericalsimulation and theory becomes possibleprobably for the rst time with the arrival

of Hinode. We are entering a golden age

in solar physics, and believe that progressin solar physics brings us with much betterunderstating on the magnetic universe towhich we all belong.

ACKNOWLEDGEMENT

The author expresses sincere thanks to theISAS/JAXA Solar-B launch team headedby Y. Morita for their exceptional achieve-ment. Hinode is a Japanese missiondeveloped and launched by ISAS/JAXA,collaborating with NAOJ as a domesticpartner and NASA and STFC (UK) asinternational partners.

I would like to thank Drs. Satoshi Ma-suda and Louise Harra for providing somedescription in the paper [31, 32].

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Fig. 8: Large solar are captured by SOT on 13 December 2006. Two-Ribbonstructure and some of post-are loops between the two ribbons are clearly seen.(Courtesy of NAOJ, JAXA, and NASA.)

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