Opening Talk

Kazunari ShibataKwasan 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

• 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 reconnectionin flares was discovered by Yohkoh

Masuda et al. 1994 Tsuneta et al. 1992

Shibata et al. 1995

Loop top hard X-ray sources

Plasmoid ejections

small flares ~ 10^9 cm(Ohyama)

large flares~ 10^10 cm(Hudson)

coronal mass ejections(CMEs) from larger flares/arcades ~ 10^11 cm(Dere)

Unified model

downflow

• Discovered with Yohkoh soft X-ray telescope(McKenzie, Hudson,,,)

• TRACE observations

(Innes, Asai,,,)

Yohkoh/SXT : McKenzie 2000

Shrinking motion of reconnected loop ?

Downward plasmoid orreconnetion outflow ?

jets, jets, jets, ,,, solar atmosphere is much more dynamic than had been tho

ught, and full of jets, nanoflares, and reconnection

SOHO/CDS (Pike&Mason)

TRACE (Alexander and Fletcher )

Hida (Hα) （ Kurokawa et al ）

Yohkoh(Shibata, Shimojo,,,)

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

１MK ３MK １０MK

To observe energy release processes in the corona

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

Emerging bipole

jet

Loop oscillation

Reconnection inflow

Turbulence?

Evaporation flow

Reconnection outflow

Te & ne along a coronal loop

To observe true velocity fieldIn the corona andtransition region

（ 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

Solar flare

MagnetosphericAurora-substorm

Laboratoryreconnection

Tokamak disruption

Protostellarflare

time(hour)

time(hour)

MagneticField

strength

time(μsec)

time(sec)

time 105 sec

X-rayintensity

X-rayintensity

MagneticField

strength

Electrontemperature

Various “Flares” (Reconnection Phenomena)

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 !