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

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

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

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.

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.

Why we have Solar B ? What is Solar B ?

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

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

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)

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

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)

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 ?

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

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

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

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)

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

space weather The Earth is badly affected by the Sun

Basic MHD processes in stars and disks

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

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

Please enjoy scientific discussion and Kyoto !