Department of Astronomy, Nanjing University, Nanjing 210093, China C. Fang, M. D. Ding, P. F. Chen Possible collaboration between Solar-B and the facilities.

Department of Astronomy,

Nanjing University,

Nanjing 210093, China

C. Fang, M. D. Ding, P. F. Chen

Possible collaboration between Solar-B and the facilities of Nanjing University

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

Liu, Ding, Fang, : 2001, ApJ, 563, L169

Li & Ding, 2004, ApJ, 606, 583

2. A near infrared WLF

3. Nonthermal signatures

Ding & Fang: 1995, A&AS, 563, L169

From Nanjing to Kunming

Fuxian Lake

撫仙湖

31.8 km

New Site: Fuxian LakeLocation: 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

200mm

1-4 frames per minute

Credit: BBSO

Λ360.0 nm and

425.0 nm

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

Ribbon motion recon. rate Fast fluctuations: elementary burstsWang, H. et al. (2000)

H-1.3 Å

Qiu et al. (2004)

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.There should be more!

1. They are short-lived;

2. Few telescopes tailored for that purpose.

Hudson (2005): All flares are WLFs. (Trace …) Need be checked

carefully!A catalog including types I & II WLFs

(Fang & Ding 1995) will be provided.

Flare-associated Sprays, Surges, …

Kurokawa et al. (1987)

Jibben & C. Canfield (2004)

Handedness distribution,Helicity transport,

…

right-handedleft-handed

H center, ±0.5 Å

Filament Eruptions near CME Onset

H center, ±0.5 Å

LOS velocityMorimoto & Kurokawa (2003)

Chen & Shibata (2000)

Zhang et al. (2001)

1. To monitor the onset of filament eruptions;

2. To clarify the relationship btw CMEs and flares.

CME-associated Waves/Brightenings

He wavesGilbert et al. (2004)

EIT wavesThompson et al. (1998)

Coronal wavesHarra & Sterling (2003)

Moreton Waves

H+0.8ÅCredit: Kyoto University colleagues Ha+0.4 Å

Ha-0.4 ÅH ± 0.4 Å may be the best

Chen, Fang, Ding (2005, Space Sci. Rev.)

Chen et al. (2002, ApJ, 572, L99)

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)

775 km/s

250 km/s

Coordinated observations will finally resolve the dispute

Ellerman Bombs, Microflares, Dark points, Coronal Holes, …

EBs,MF

CHs

DPs Harvey (1984)

Chen et al. (2001, ChJAA, 1, 177)

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

He 10830 SXR

Fang et al. (2006, ApJ, in press)

Filament Oscillations

Eto et al. (2002)

-0.8 Å H core +0.8 Å

Prominence seismology will be enhanced!

Operations

Partner in construction and operations:

YNO: NAOC/Yunnan Observatory

Commencement: 2008

Data Policy: open

Observation Modes

Partial Disk Mode (PDM, better

than 1“, FOV:10’)

Full Disk Mode (FDM)

Introduction of SMESE (SMall Explorer for Solar Eruptions)

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

A Franco-Chinese small satellite

To observe the solar flares and CMEs

for the next solar maximum

Main Scientific Objectives

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)

Instruments

MYRIAD

DESIR

LYOT

HEBS

Guide Telescope

SMESE Payload

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, ……

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!

2. SMESE can provide Lyαimages, Lyαcoronagraphs,

EUV images, HXR and γ-ray flux with high temporal

resolution.

谢 谢！谢 谢！ThankThankss ！！