Opening Talk Kazunari Shibata Kwasan and Hida Observatories Kyoto University.
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Transcript of 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
• 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.
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
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