Transcript ONSET_collaboration

Possible collaboration between
Solar-B and the facilities of
Nanjing University
C. Fang, M. D. Ding, P. F. Chen
Department of Astronomy,
Nanjing University,
Nanjing 210093, China
Outline
1. Observation History in Nanjing University
2. Introduction to the New Telescope
3. Scientific Objectives and Possible
Collaborations
4. SMESE- a Franco-Chinese Small Satellite
5. Summary
Solar Tower (since 1980)
Multi-wavelength
2-Dimensional
Spectrograph
H
Ca II (K, 8642)
He I 10830
Highlights of the Achievements
1. More accurate atmospheric
models for solar flares
Ding & Fang: 1995, A&AS, 563, L169
2. A near infrared WLF
Liu, Ding, Fang, : 2001, ApJ, 563, L169
3. Nonthermal signatures
Li & Ding, 2004, ApJ, 606, 583
From Nanjing to Kunming
31.8 km
Fuxian Lake
撫仙湖
New Site: Fuxian Lake
Location: E102º57´, N24º38´ (60 km from Kunming)
Altitude: 1722 m
Total area: 212 km2
Second deepest lake
in China, mean depth
is 87m.
Main Components
Three Tubes
 H 6563
 He I 10830
 White light
Designed by NIAOT
Name of the Telescope
ONSET:
Optical and NIR Solar Eruption Tracer
H Filtergraph
H center, ±0.5 Å
275mm
1-120 frames per minute
Credit: BBSO
He I 10830 Filtergraph
He I 1083.0nm center
275mm
1 frame per minute
Credit: MLO
White Light Filtergraph
Λ360.0 nm and
425.0 nm
200mm
1-4 frames per minute
Credit: BBSO
Scientific Objectives and
Possible Collaborations
Flare dynamics
H and high-T flares, WLF patrol, …
CME onset and wave survey
He wave/brightening, Moreton waves, EIT wave,
filament eruptions, …
Structures and evolution of various activities
Coronal holes, small activities, microflares,
filament oscillation, …
Flare Ribbons and Dynamics
H-1.3 Å
Ribbon motion recon. rate
Qiu et al. (2004)
Fast fluctuations: elementary bursts
Wang, H. et al. (2000)
To derive non-thermal parameters and
dynamical processes of flares
through ground-based and space observations!
White Light Flare Patrol
Since 1859, only ~110
WLFs have been observed.
1. They are short-lived;
2. Few telescopes tailored for that purpose.
Hudson (2005): All flares are WLFs.
(Trace …)
A catalog including types I & II WLFs
(Fang & Ding 1995) will be provided.
Flare-associated
Sprays, Surges, …
H center, ±0.5 Å
Kurokawa et al. (1987)
left-handed
right-handed
Jibben & C. Canfield (2004)
Handedness distribution,
Helicity transport,
…
Filament Eruptions near CME Onset
H center, ±0.5 Å
Morimoto & Kurokawa (2003)
LOS velocity
1. To monitor the onset of filament
eruptions;
Chen & Shibata (2000)
Zhang et al. (2001)
2. To clarify the relationship btw
CMEs and flares.
CME-associated Waves/Brightenings
EIT waves
Thompson et al. (1998)
He waves
Gilbert et al. (2004)
Coronal waves
Harra & Sterling (2003)
Moreton Waves
Chen et al. (2002, ApJ, 572, L99)
H+0.8Å
Credit: Kyoto University colleagues
H ± 0.4 Å may be the best
Chen, Fang, Ding (2005, Space
Sci. Rev.)
Ha+0.4 Å
Ha-0.4 Å
Moreton, EIT, X-ray and He Waves will be recorded,
which is crucial for understanding CMEs
Dispute on EIT wave mechanism
Fast-mode wave model
Non-wave model
Thompson et al. (1998)
Wang, Y. -M. (2000)
Wu et al. (2001)
……
Delannee & Aulannier (2000)
Chen et al. (2002, ApJ, 572, L99)
250 km/s
775 km/s
Coordinated observations
will finally resolve the dispute
Ellerman Bombs, Microflares,
Dark points, Coronal Holes, …
EBs,
MF
Chen et al. (2001, ChJAA, 1, 177)
Harvey (1984)
DPs
He 10830
CHs
Fang et al. (2006, ApJ, in press)
SXR
Coordinated observations with SOT,
XRT and EIS will be very useful to
understand the mechanism for small
scale activities and magnetic
reconnection in the solar atmosphere
and the source of the fast solar wind
Filament Oscillations
-0.8 Å
H core
+0.8 Å
Eto et al. (2002)
Prominence seismology will be enhanced!
Operations
Commencement: 2008
Data Policy:
open
Observation Modes
 Partial Disk Mode (PDM, better
than 1“, FOV:10’)
 Full Disk Mode (FDM)
Partner in construction and operations:
YNO:
NAOC/Yunnan Observatory
Introduction of SMESE
(SMall Explorer for Solar Eruptions)
A Franco-Chinese small satellite
Institut d’Astrophysique Spatiale, CNRS, France
Observatoire de Paris, LESIA, France
Purple Mountain Observatory, CAS, China
Nanjing University, China
Center for Space Research and applied Research, CAS, China
National Astronomical Observatory, CAS, China
Main Scientific Objectives
To observe the solar flares and CMEs
for the next solar maximum
Instruments
Lyman-alpha disc imager (up to 1.15R¤)
Lyman-alpha coronograph (1.1-2.5R¤)
EUV (FeXII 19.5 nm) disc imager
Far Infrared telescope (35 & 150 m)
X-ray spectrometer (10-300 keV)
Gamma-ray spectrometer (0.2-600 MeV)
SMESE Payload
Guide
Telescope
DESIR
LYOT
HEBS
MYRIAD
Main parameters






Total weight of payloads: 56 kg
Total power consumption: 90 watt
Data rate: 31Gb per day
Dawn-dusk sun-synchronous orbit
Altidute: 700 Km
Launch time: 2010 - 2011
Prospects
Coordinated observations with solar-B
will greatly contribute to the study of
solar flares and CMEs
Summary
1. ONSET can monitor the onset of CMEs, detect various
activities with different scales, conduct the H, He and
Wight light patrol, ……
2. SMESE can provide Lyαimages, Lyαcoronagraphs,
EUV images, HXR and γ-ray flux with high temporal
resolution.
3. Coordinated observations with SOT, XRT and
EIS will be greatly desirable!
4. Data center will be installed in Nanjing University
and IAS in France. You are encouraged to use the
data!
谢 谢！
Thanks！