Report fromHigh Throughput UV/EUV
Spectroscopy sub-WG
Toshifumi Shimizu (ISAS/JAXA)
high throughput UV/EUV spectroscopy
sub-WG

20 Jan 20101

High throughput UV/EUV spectrograph- Instrument for quantitative investigations on the physics
of dynamics with UV/EUV spectroscopy -Objective:
Quantitatively observe energy flows at dynamic times scale over the entire
atmosphere from chromosphere to hot corona with high resolution, highthroughput spectroscopy in UV-EUV and understand physics of dynamics andheating.

Study Activities:• International high-throughput UV/EUV spectroscopy sub-WG working forscience & feasibility investigation of the instrument.
Luca Teriaca (MPS)
Udo Schuehle (MPS) - instrument expert
Louise Harra (MSSL)
George Doschek (NRL, co-chair for this sub WG)
Clarence Korendyke (NRL) - instrument expert
Joe Davila (NASA/GSFC)
Ted Tarbell (LMSAL)
Hiroaki Isobe (Kyoto University)
Shinsuke Imada (ISAS/JAXA)
Tetsuya Watanabe (NAOJ)
Hirohisa Hara (NAOJ)
20 thisJan sub2010
Toshifumi Shimizu (ISAS/JAXA, Chair forWG)

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Quantitative understanding of highly dynamic atmospherewaves, turbulence, magnetic reconnection
Hinode discoveries
Waves in prominence
Chromospherictransition region
jets due toreconnection
Waves alongspicules

コロナ

Slow solar wind

遷移層

Polar kG fields

Supersonic downflow
Convective collapse
彩層Penumbral
micro-jets
Magnetic velocity
Fluctuation
Local dynamo
process

Ubiquitous
Horizontal20fields
Jan 2010

High coronalturbulence

33

Rutten, R., ASP-CS, 184, 181, 1999

High throughput UV/EUV spectrograph- Instrument for quantitative investigations on the physics
of dynamics with UV/EUV spectroscopy -• B案衛星に搭載を想定した大型の分光器–目指す装置方向性–サイエンスケース• A案衛星に載せる小型化分光器
20 Jan 2010

4

B案衛星
High throughput UV/EUV spectrograph• 将来の分光望遠鏡の方向性（装置に求める性能）
1.

高い時間分解能(頻度)2.

広い温度範囲をくまなくカバー

3.

高い解像度

4.

可能な限り広い視野

5.

低散乱光での観測低いEM領域の診断を可能に。磁気リコネクショ
ン領域、オフリム上空(太陽風加速, 衝撃波)など。

6.

他望遠鏡との協調ダイナミックな活動の物理的診断。既存の分光望遠鏡に比べ1桁以上高いスループット。

彩層(1万度)から高温コロナ・フレア(1000万度)のプラズマを同時診断。多温度プラズマから成る構造を理解
ひのでSOTが分解した彩層磁場構造（スピキュール等）の上空への結びつきを確実に特定。0.5秒角以下 (0.2-0.3”目標)。

高解像度の視野は~5x5分角以下に制限されるが、低解像度では広い視野をカバー。宇宙天気とのリンク。

他の搭載望遠鏡からの観測データと確実な比20 Jan 20105
較研究を可能に。コアラインメント。

High throughput UV/EUV spectrograph
Performance much improved from previous instruments
Strawman instrument schematic
大型分光望遠鏡の雛形概念図

solarradiation

Primary Mirror
30~40cm
Focal Plane Detectors(Solar-blind intensified
APS or CCD)
Entrance Slit•

Grating(TVLS)

By removing metal filters with solar-blind intensified detector, having
minimum numbers of optics and ~30cm aperture, we expect >10
improvement in effective area from EIS and SUMER.
20 Jan 20106

High throughput UV/EUV spectrograph
Performance much improved from previous instruments
ロケット実験EUNIS用センサ部（例）TVLS (ToroidalVaried Line-Space)

グレーティングにより、光学拡大率を持つことが可能に。
サブ秒角の解像度の実現が可能に。
UV光に感度をもつマイクロチャンネルプレート(MCP)を使用。太陽可視・赤外光に感度をなくす設計で、金属プレフィルタ(の厚み・枚数)を削除する。センサはCCDかAPS（高速読み出しに利点）が候補。
20 Jan 20107

High throughput UV/EUV spectrograph
Performance much improved from previous instruments
Effective area of the strawman instrument (solid lines).
Previous comparable effective areas for EIS, CDS and SUMER areplotted for comparison.

20 Jan 20108

UVラインのフォトン数(輝線形成温度の関数で)各点が雛形の観測波長内の各ラインで期待されるフォトン数。空間サンプリング0.33”にて。>100フォトンで速度診断が可能。

平均的な静穏領域

SUMER相当

平均的な活動領域EIS相当

フレアプラズマ•

Temporal resolution can be more improved with observing bright lines,
which are formed in wide temperature range in 104-107 K.

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既存の装置 Hinode/EIS

20 Jan 201010

EIS intensity and velocity maps to show plasma outflows from the edges of the active region, June 27, 2009, Credit Deb Baker

既存の装置 Hinode/EIS:
Insufficient performance• EIS is a very good instrument, but ….
• Need long exposure for the quiet Sun
observations. ~100 s required.
• It is also true for some topic of active region
observations~ 1hr scan duration for 4x4 arcmin2 for line
width measurements• Low spectral resolution for line profile analysis• Weak TR lines in the EIS wavelength band
• We now know that there are unresolved
structures.
20 Jan 201011

VUV spectrograph SUMER on SOHO
Spectral coverage from 800 to1600A, where spectral lines from TR is rich.
raster scanof sunspot:vis 6330A

raster scanof polar region:cont. ~1250A

N V 1238A

Fe XII 1242A

Mg X 609AO V 629A

Fe XII 1242A

EISで弱い遷移層の診断を可能とす
る輝線があるが、時間分解能・空間分解能が不十分。

N V 1238A

20 Jan 2010
C I 1249A

12

既存の装置 Hinode/EIS:
Insufficient performance• EIS is a very good instrument, but ….
• Need long exposure for the quiet Sun
observations. ~100 s required.
• It is also true for some topic of active region
observations~ 1hr scan duration for 4x4 arcmin2 for line
width measurements• Low spectral resolution for line profile analysis• Weak TR lines in the EIS wavelength band
• We now know that there are unresolvedstructures.
20 Jan 201013

UnveilingUnveilingthe
theMicrophysics
Microphysicsof
ofthe
theSolar
SolarCorona
Corona•Particle acceleration•Magnetic reconnection•Ion-cyclotron wave heating•Turbulent cascades•Non-Maxwellian distributions
SOHO/EIT: 2.6” pixels

Seeing the microphysics requires
high spatial and spectral resolution
coupled observations from thephotosphere into the corona

TRACE: 0.5” pixels

5,800 km

Yohkoh: 2.45” pixels

Elementary heating eventin a polar coronal hole.
This event is clearlyunresolved at ~EIS/TRACE spatial resolution.

Hinode/EIS: 1” pixels

20 Jan 2010

TRACE: 0.5” pixels

Plan B Solar-C: 0.1” – 0.3” spatial
resolution will provide an exact
match from the photosphere into
the corona, thus allowing resolutionof elementary heating events andtraceability of footpoint mechanicalenergy into the coronal magnetic
field and into consequent plasma
heating.
14

Science Goals
•

•

•
•
•
•

Trace energy flow at natural dynamic solar time scales over alarge dynamic range from the photosphere into the corona
through small spatial-scale elementary solar structures anddetermine the resulting large-scale structures (Understand thephysics of the beta = 1 region)
Understand physical processes such as magnetic dissipation
and reconnection in astrophysical plasmas, under a wide
variety of physical conditions. (Measure the magnetic field in
the chromosphere; make accurate extrapolations of the coronalfield)
Understand and spatially resolve elementary atmosphericstructures over each temperature domain of the atmosphereand determine how they are created and evolve
Understand how small-scale physical processes initiate large
scale dynamic phenomena creating space weather
Understand how physical processes alter coronal properties
such as variations in its composition (put in for supporting insitu measurements)
Particle acceleration???
20 Jan 201015

新しいサイエンスの窓への期待• 磁気エネルギ開放過程(磁気リコネクション)の真髄に迫る• 彩層~遷移層~コロナの磁気カップリング– コロナ加熱： エネルギー・物質輸送– 磁気大気の素構造 彩層磁場

• オフリム観測： 太陽風加速、衝撃波面• 宇宙天気研究への展開– 大きな構造・現象(CME, フレア, 太陽風)とミクロな物理過程
20 Jan 201016

磁気エネルギ開放過程(磁気リコネクション)の真髄に迫る ( 今田講演)
Exploring physics of magnetic It is a key point toinvestigate simultaneously
dissipation (reconnection)
Why the dissipation is so fast?

the broad temperature
range.

Heating problem(Corona, Chromosphere)

Magnetic reconnections
in partially-ionizedplasma (chromosphere)

What (boundary, plasma
condition) control the rate?

For understanding
astrophysical plasma
It is a key point to make direct
measurements of plasma in the area
close to diffusion region.

For understanding nature ofdynamics in the solar
plasma, flares, and CMEs.
It is a key point to make highcadence measurements fordynamics.

20 Jan 2010

Fundamental structures ofenergy flows in dynamic timescales?

nanoflare

Magnetic patches withsingle polarity

Their connection to magnetic
17
fields in the chromosphere/photosphere?

時間・空間分解能の向上で、
1) 磁気リコネクションによって一時的に生成される非平Te~650eV(750衡プラズマの状態万度)に対応す
2) 電子速度の非マクスウェ
る電子温度分布
ル分布の情報3) イオン温度分布 (Imada etal 2008)
Line Spectra on Fe XIVなどを探ることができる。 logT (K)=6.3, N =1011cm-3, T =T , N =0.83N
eepepen = 1 (maxwellian)n = 3 (non-maxwellian)

20 Jan 2010

(Watanabe, Kato, & Yamamoto, 2008)

18

彩層~遷移層~コロナの磁気カップリング

Understanding elementary atmospheric structures• Understand and spatially resolve elementary magnetic
atmospheric structures over each temperature domain of theatmosphere and determine how they are dynamically createdand evolve and responsible for heating and dynamics.
In the corona

White lines:
Magnetic field lines•

A signature caused by highly
blueshifted component (>100km/s)
was discovered with EIS observations,which may be a signature ofnanoflares at the base of coronal loops

DiskCenter (C)Limb (L)(Hara et al. 2008)20 Jan 201019

Important roles of weak magnetic
fields in chromosphere

Horizontal fields (yellow)
overlapped on granule image•

Hinode revealed that small-scale horizontal
fields exist ubiquitously and behave
dynamically in the photosphere (Lites et. al. 2007,Ishikawa et al. 2008)

20,000• Horizontal magnetic fields may play important
km roles in forming the magnetic structures in thechromosphere.
•Ishikawa et al. (2008)

They may produce nanoflares (magenticreconnections) and resultant MHD waves,which are important in understanding heating
and dynamics of the atmosphere.

Vertical field not shown here

Tip of icebergs

Convectivegas flows

Horizontally oriented 20 Jan 2010
magnetic flux tube

Isobe et al. (2008)
wave20彩層~遷移層~コロナの磁気カップリング

Trace energy and mass flows at dynamic time scales•Quantitatively understand energy and mass flows at dynamic timescales over a large dynamic range from the photosphere into thecorona through small spatial-scale elementary solar structures.

Magnetic dynamic structure
In the chromosphere by SOTEIS Fe XII 195 (~1.4MK)
Radiance

Doppler

FWHM

TRACE 171

両者を観測から如何に結びつけるか20 Jan 2010
 空間・時間分解能・温度カバー

21

オフリム観測(1)Sources of the solar fast wind
• 極域： 高速太陽風加速におけるplumes, interplumesの役割は？
• VUV (>1000A)スペクトル観測による診断方法• Doppler shift• Doppler dimming

Teriaca et al. 2003

Solar-C (MPS評価)• We need a very good control of thestray-light (micro-roughness ~2 Ǻrms).
20 Jan 201022

Doppler Dimming
Teriaca et al. 2003

• Allows to determine the radial
component of the plasma
outflow velocity from theanalysis of off-limb spectra.
• Line emission mechanisms– Electron impact excitation(collisional component).
– Resonant absorption of disk
radiation (radiative component).
– Example, Ratio of O VI 1032A andO VI 1037A, Ly• 比は、主にNeとアウトフロー速度の関数• 結果、４者４様• S/Nの不足, 太陽大気ダイナミックスとの関係  High throughput
20 Jan 2010

O VI
SUMER

UVCSLy23

オフリム観測（２）Shocks/Energetic Particles?
• Type II radio eventsare generated bycoronal shocks• Most are below 3Rsun• Shocks passing
through FOV visible
as narrow hightemperature events
20 Jan 2010

SCSGopalswamy

24

宇宙天気現象への展開• How microphysics are linked to resulting large‐scale
structures (such as corona and solar winds) anddynamics (such as flares and CME)?

20 Jan 201025

Major jumps from IRIS?
• IRIS (Interface Region Imaging Spectrograph) is approved forlaunch in 2012.
– IRIS diagnoses spectral lines in 120‐280nm with 0.3” and 1‐5s cadence todiscover how an outer stellar atmosphere is energized.
– The spectral lines observed with IRIS are suitable to explore the interface
between upper chromosphere and lower transition region.

• Still major jumps from IRIS, because the S‐C plan‐B canprovide unique observations which have never been realized:(IRIS‐Hinodeデータを見る必要はあるが、現時点で)– Quantitative measurements of magnetic fields in the chromosphere– EUV/UV spectral lines used in Solar‐C spectrograph will seamlessly cover fromchromospheric temperature through the coronal temperature with 0.1‐0.5”
and 1‐5 s cadence.
– Energy spectral (thermal and non‐thermal) diagnostics in 106‐107 K plasma forflares and active region dynamics.
20 Jan 201026

20 Jan 2010

27

A案衛星
High throughput UV/EUV spectrograph• A案衛星に載せる小型分光器• ESA/NASA Solar Orbiter（SO）の搭載機器の一つとして選ばれたSPICE (Spectral Imaging of theCoronal Environment, PI: D.Hassler)とほとんど同じものを想定。
• B案衛星搭載の大型分光器を長さ1m規模に小型がしたもの

20 Jan 2010

28

SPICE on Solar Orbiter••••

駆動機構付きオフセット主鏡、スリット、TVLSグレーティング、intensified APS
主鏡の開口径 5cm x 5cm
FOV 16‐17 arcmin (1Kx1K), spatial 1”@0.3AU
観測波長帯 2バンド：702‐792 A
972‐1050A (2nd order 486‐525A)– 強輝線：C III 977 (logT=4.8),
O VI 1032 (logT=5.5)

Ne VIII 770 (logT=5.8)
Si XII 521 (logT=6.3)
他にも多数の輝線あり•••

速度サンプリング 23 km/s/pixel@1000A~EIS長波長バンド程度と同等
熱環境が大きく変動するため、焦点調節機構をもつ
遮光板 (off‐limb occulter) for オフリム観測 (>3.0Rsの観測)
20 Jan 201029

http://solarorbiter3.oato.inaf.it/Presentazioni/so3_2805_hassler_talk.pdf

20 Jan 2010

30

A案衛星の利点は？
• UVスペクトル観測の観点からも、極を見る観測は、極域コロナホール(高速太陽風の源のダイナミックス)の理解のための観測を可能とする。極を見るミッションは科学的に重要。
• しかし、A案衛星は、Solar orbiterに対して大きなジャンプの期待は小さい。また、下記の利点から失うものがある。
– その場観測との連携の不足– 太陽自転速度と同期しない観測 (SOは太陽自転と同期した観測を行う)– 約1/3の解像度• 一方で、衛星リソースから、A案の利点がある可能性– SO 100Kbps観測 数日~10日/orbitと期間が限定。SPICEは16Kbps程度。 データ量、連続観測の点でA案に利点• A案スペクトル観測は、Solar Orbiterの実現如何に依存 (世界で２つ作るのは...)
20 Jan 201031

High Throughput UV/EUV
Spectrograph• sWGの一致した意見として、2010年代後半に早急に、大型分光装置を実現させたい。
• 鍵となる性能として。
– 高スループット、高時間・空間分解能化。EIS+SUMERに対して１桁以上の向上可能– 彩層からコロナ・フレアまで強輝線で抜けのないカバー。
観測波長(詳細選択は未)としてはEIS+SUMER合体版。
– 技術的には、現時点では実現可能な範囲。

• IRIS(2012)からのジャンプは、多少なやみのたね。
• A案への小型分光装置は、Solar Orbiterの実現如何に依存。
20 Jan 201032