Title: Opening Talk
1Opening Talk
- Kazunari Shibata
- Kwasan and Hida Observatories
- Kyoto University
2SOC 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
3Organization
- This meeting is organized by Kwasan and Hida
Observatories of Kyoto University
Kwasan Obs
Hida Obs
4Sponsors
- 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.
5Objective 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.
6Why we have Solar B ?What is Solar B ?
7Yohkoh (Solar A) observations of Solar Corona
(1991-2001)
- Soft X-ray
- (1 keV)
- 2MK-10MK
8Various evidence of magnetic reconnectionin
flares was discovered by Yohkoh
Loop top hard X-ray sources
Masuda et al. 1994
Tsuneta et al. 1992
Shibata et al. 1995
9Plasmoid ejections
Unified model
coronal mass ejections (CMEs) from larger
flares/arcades 1011 cm (Dere)
large flares 1010 cm (Hudson)
small flares 109 cm (Ohyama)
10downflow
- 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 jets, jets, jets, ,,, solar atmosphere is
much more dynamic than had been thought, and full
of jets, nanoflares, and reconnection
Hida (Ha) (Kurokawa et al)
Yohkoh (Shibata, Shimojo,,,)
TRACE (Alexander and Fletcher )
SOHO/CDS (PikeMason)
12Remaining 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 ?
13Solar-B Mission
- Solar Optical Telescope (SOT)
- X-Ray Telescope (XRT)
- EUV Imaging Spectrometer (EIS)
- Launch Date 2006 summer
- Mission Lifetime gt 3 years
- Orbit Polar, Sun Synchronous
- Scientific objective
- coronal heating mechanism
- elementary MHD processes such as magnetic
reconnection
14Solar B / Solar Optical Telescope (SOT)
- 50 cm Aplanatic Gregorian telescope
- Focal Plane Package (Filtergram
Spectro-polarimeter) - gt 0.2 arcsec resolution 150 km
- vector magnetic field measurements
To observe energy generation and transport
processes from photosphere to corona
15Solar B / X-Ray Telescope (XRT)
- Grazing-Incidence telescope
- CCD Camera
- gt 1 arcsec resolution 700 km temperature
1 30 MK
To observe energy release processes in the corona
3MK
1MK
10MK
16Solar B / EUV Imaging Spectrometer (EIS)
- 15 cm Offset Parabolic Mirror Slit/Slot
Multilayer Grating - gt 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)
17Importance 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
18space weather
The Earth is badly affected by the Sun
19Basic MHD processes in stars and disks
20Various 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
21Previous 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
22Please enjoy scientific discussion and Kyoto !