1. Kazunari Shibata Kwasan and Hida Observatories Kyoto University
Opening Talk
Kazunari Shibata
Kwasan and Hida Observatories
Kyoto University

2. SOC and LOC
Scientific Organizing Committee: K. Shibata (co-chair), T. Sakurai (co-chair), M. Carlsson, J.L. Culhane, J. Davis, L. Golub, H.S. Hudson, T. Kosugi, B. Lites, T. Sekii, K. Shibasaki, A.M. Title, S. Tsuneta, T. Watanabe, T. Yokoyama
Local Organizing Committee: K. Shibata (chair), H. Kurokawa, R. Kitai, S. Masuda, S. Nagata, S. Ueno, T. Miyagoshi, T. Ishii, S. Tanuma, H. Isobe, A. Asai, M. Shimojo, H. Tonooka, C. Sampa, M. Oka, M. Uemura

3. Organization Kwasan Obs Hida Obs
This meeting is organized by Kwasan and Hida Observatories of Kyoto University
Kwasan Obs
Hida Obs

4. Sponsors
Grant-in-Aid for the 21st Century COE "Center for Diversity and Universality in Physics“ of Kyoto University (PI: Prof. K. Koyama)
Yukawa Institute for Theoretical Physics of Kyoto University
Solar Terrestrial Environment Laboratory of Nagoya University.

5. Objective of this meeting
The Solar-B satellite will be launched next year (2006 summer) by ISAS/JAXA as an international collaboration project with USA (NASA), UK (PPARC), and ESA.
We are now about one year before the launch and it is therefore timely to discuss basic scientific objectives, possible observing proposals and programs of the Solar-B mission.

6. Why we have Solar B ? What is Solar B ?

7. Yohkoh (Solar A) observations of Solar Corona (1991-2001)
Soft X-ray
（~1 keV)
2MK-10MK

8. Various evidence of magnetic reconnection in flares was discovered by Yohkoh
Loop top hard X-ray sources
Solar corona is much more dynamic than had been thought, and is full of jets, microflares, and mass ejections
Various evidence of magnetic reconnection was discovered in flares and CMEs, so that reconnection model of flares has been established
Masuda et al. 1994
Tsuneta et al. 1992
Shibata et al. 1995

9. Plasmoid ejections Unified model coronal mass ejections large flares
(CMEs) from larger flares/arcades
~ 10^11 cm
(Dere)
large flares
~ 10^10 cm
(Hudson)
small flares
~ 10^9 cm
(Ohyama)

10. downflow Discovered with Yohkoh soft X-ray telescope
(McKenzie, Hudson,,,)
TRACE observations
(Innes, Asai,,,)
Shrinking motion of reconnected loop ?
Downward plasmoid or
reconnetion outflow ?
Yohkoh/SXT : McKenzie 2000

11. Hida (Hα) （Kurokawa et al）
jets, jets, jets, ,,, solar atmosphere is much more dynamic than had been thought, and full of jets, nanoflares, and reconnection
Hida (Hα) （Kurokawa et al）
Yohkoh
(Shibata, Shimojo,,,)
TRACE (Alexander
and Fletcher )
SOHO/CDS (Pike&Mason)

12. Remaining Questions What is the coronal heating mechanism ?
Nanoflare or Alfven wave ?
Solar wind acceleration mechanism ?
What is the elementary MHD processes such as reconnection ?
Velocity of reconnection Inflow / outflow ?
What determines reconnection rate ?
What is the triggering mechanism of flares and CMEs ?
What is the origin of magnetic field and activity ?
Subsurface magnetic and velocity field ?
Photosphere-corona magnetic coupling ?

13. Solar-B Mission Solar Optical Telescope (SOT) X-Ray Telescope (XRT)
EUV Imaging Spectrometer (EIS)
Launch Date: 2006 summer
Mission Lifetime: > 3 years
Orbit: Polar, Sun Synchronous
Scientific objective
coronal heating mechanism
elementary MHD processes such as magnetic reconnection

14. Solar B / Solar Optical Telescope (SOT)
50 cm Aplanatic Gregorian telescope
Focal Plane Package (Filtergram + Spectro-polarimeter)
=> 0.2 arcsec resolution; ～150 km
vector magnetic field measurements
To observe energy generation and transport processes from photosphere to corona

15. Solar B / X-Ray Telescope (XRT)
Grazing-Incidence telescope
CCD Camera
=> 1 arcsec resolution; ～700 km temperature : 1 – 30 MK
To observe energy release processes in the corona
３MK
１MK
１０MK

16. Solar B / EUV Imaging Spectrometer (EIS)
15 cm Offset Parabolic Mirror Slit/Slot & Multilayer Grating
=> 20 km/s nonthermal motion
2 arcsec resolution : ～1400 km
Temperature : 0.1 – 20 MK
To observe true velocity field
In the corona and
transition region
Te & ne
along a coronal loop
Reconnection outflow
Emerging bipole
Reconnection inflow
jet
Turbulence?
Evaporation flow
Loop oscillation
（Hara)

17. Importance of Solar B
Basis of space weather research (cf CAWSES (= Climate And Weather of the Sun-Earth System) project)
Laboratory of Astrophysics
Basic Plasma Physics

18. space weather
The Earth is badly affected by the Sun

19. Basic MHD processes in stars and disks

20. Various “Flares” (Reconnection Phenomena)
X-ray
intensity
Solar flare
time(hour)
Magnetic
Field
strength
Magnetospheric
Aurora-substorm
time(hour)
Magnetic
Field
strength
Laboratory
reconnection
time(μsec)
Tokamak
disruption
Electron
temperature
time(sec)
X-ray
intensity
Protostellar
flare
time
105 sec

21. Previous Solar B science meeting
1st : 1999 Dec 9-10, Sagamihara, Japan
2nd : 2000 Dec 4-6, Sagamihara, Japan
3rd : 2002 Jan 25-26, Kona, Hawaii, USA
4th : 2003 Feb 3-5, ISAS/NAOJ, Japan
5th : 2003 Nov 12-14, Roppongi, Tokyo, Japan
6th : 2005 Nov 8-11, Kyoto, Japan
First Solar B meeting in Kyoto

22. Please enjoy scientific discussion and Kyoto !