DST将来計画と高時間分解能撮像観測
京大・理・附属天文台
北井礼三郎

太陽観測のベクトル
時間分解能
Solar-B
波長分解能

空間分解能

地上AO
大口径

多点同時分光広視野

波長レンジ

多波長同時分光
近赤外分光＊Targetting 機動性＊大容量データ取得

長時間スパン
Solar-B

粒子加速の問題• 太陽大気での粒子加速＊どこで加速され＊どのように伝播し＊どのように散逸されるか• Elementary Burst （Hαカーネル高時間分解観測）＊Duration （≦0.3秒）⇒ 加速領域のサイズ導出⇒ 格段に短い？
＊Location of acceleration⇒ ＨＸＲによるTime-of-flight 解析⇒ 彩層突入点の同定
Aschwanden (1996)Kurokawa, Takakura, Ohki•••Comparison of Hα-1.0Å light curve (temporal resolution 1s) withthat of Hinotori HXRFootpoints of a flare loop (Hαkernels) synchronously brighten.
Time profiles of Hα and HXR show good time correspondence
in impulsive phase.
⇒ Electron Beam Heating of ChromosphereHigh time resolution observations of the solar flare Ha emission
K. Radziszewski, P. Rudawy, K.J.H. Phillips, B.R. Dennis
Advances in Space Research 37 (2006) 1317–1322
•
•
•
•
•

D：53cm Coronagraph
9 Channel MSDPEEV CCD (512×512, １０bit, 70ｆ/s）
Cadence 0.04-0.05s （Limitted bylight level)
Comparison with HXR(RHESSI) andSXR(Goes)• Simultaneous HαBrighetning with HXR(Hα Integrated Intensity)•No Periodic Variation• No time delay between
light curves• Some Hα kernels show
no correnponding HXRburst

HIGH-CADENCE OBSERVATIONS OF AN IMPULSIVE FLAREHAIMIN WANG, JIONG QIU, CARSTEN DENKER, TOM SPIROCK, HANGJUN CHEN,
AND PHILIP R. GOODE
THE ASTROPHYSICAL JOURNAL, 542:1080, 2000

• Hα-1.3Å Image- 30f/s (7s obs.+15s transfer)• BATSE HXR 25-50Kev(1.02sec)

C5.7 Flare occurred at 18:09 UT
on August 23,1999 in NOAA 8673

HIGH-CADENCE OBSERVATIONS OF AN IMPULSIVE FLAREHAIMIN WANG, JIONG QIU, CARSTEN DENKER, TOM SPIROCK, HANGJUN CHEN,AND PHILIP R. GOODE
THE ASTROPHYSICAL JOURNAL, 542:1080, 2000

HIGH-CADENCE OBSERVATIONS OF AN IMPULSIVE FLAREHAIMIN WANG, JIONG QIU, CARSTEN DENKER, TOM SPIROCK, HANGJUN CHEN,AND PHILIP R. GOODE
THE ASTROPHYSICAL JOURNAL, 542:1080, 2000

• Initial brightening at the low-lying
reconnected loop (K2)
• The other kernels are footpoints ofoverlying loop (K1, K3)•• Temporal correlation – good/badcases• 0.3-0.7s fluctuations in Hα wingintensity⇒ Elementary HXR bursts• Puzzling phenomena- Pre-heating in Hα- HXR peak leads Hα blue emission
peak by 2-3 s at initial phase, while
there are no time difference at later
phase.

• Beam-heated chromosphere model- Fischer, Canfield, and McClymont (1985)- Stationary or quasi-stationary heating (several to tens of seconds)- NLTE radiative hydrodynamical simulation- Hydrogen atom : 2 bound levels+continuum• Hα simulation (NLTE Transfer )- Heated chromosphere model by sub-second beam injection( Karlicky 1990)- Hydrogen atom : 3 bound levels+continuum- Simulation of excitation and ionization of hydrogen by solving timedependent population equation- Temperature variation given by Karlicky model- Collisional processes of non-thermal electrons included⇒ (1) Slow relaxation of S, Ne (2) Initial dip of S

Hα Intensity Time Profile (Multiple Beam Injection)
DWeak BeamStrong BeamNH

• Upper layer Injection
Hα intensity peaks lag behind the beam injection (tens of seconds)• Middle layer Injection
Hα intensity gradually increases along time with darkening at
injected instances• Lower layer injection
Hα intensity simulatneously variates with the beam injection profile
Slow relaxation of excitaion and recombination
Initial dip of Hα source functionElectron Time-of-Flight measurements during the Masuda Flare,
1992 January 13
Markus J.Aschwanden et.al. APJ,464:985-998,1996
HXR flux with a time resolution 64ms(top)by BATSE/CGRO
decomposed into lower envelopes (middle) and into
pulsed components (bottom)

Electron Time-of-Flight measurements during the Masuda Flare,
1992 January 13
Markus J.Aschwanden et.al. APJ,464:985-998,1996

L’=47,000 km

L’=33,000 km

まとめ• Elementary Burst （これまでの観測結果）‐ Duration≦0.3秒‐ カーネルサイズ～１”
‐ ΔＩ
0.2%
‐ Cusp/Loop 加速? Temporal correlation? Time lag• Ｈαカーネル高時間分解能観測‐ 時間分解能10‐1 msec ⇒高速カメラ‐ 高空間分解能
0.2‖⇒Seeing ＡＯ‐ 高精度測光0.1‐0.01% ⇒大口径
⇒Scintillation AO

Atmospheric Intensity Scintillation of Stars. III.
Effects for Different Telescope Apertures
D. Dravins, L. Lindegren, E. Mezey and A. T. Young
Publications of the Astronomical Society of the Pacific, 110:610–633, 1998

Fig. 1.—Power spectral density of scintillation in telescopesof different size. The symbols are values measured on La
Palma for a sequence of small apertures.
Their fit to a sequence of synthetic spectra predicts thescintillation also in very large telescopes up to 8 m diameter.
Bold curves are for fully open apertures. A
central obscuration (secondary mirror) increases thescintillation power, while apodization decreases it for hightemporal frequencies.

END

RHESSI•

Spatial Resolution

2 ― to 100 keV
7 ― to 400 keV
36‖ above 1 MeV•Time ResolutionTens of msec for a basic image
2 seconds (half a rotation of thespacecraft) for a detailed
image