Transcript PPT

The 6th Solar-B Science Meeting
Takeo Kosugi (ISAS/JAXA, Japan)
2005 Nov. 8, Kyoto
Sun - A Magnetic Star
Various structures and dynamics,
governed by magnetic fields
The Solar Atmosphere
• Coronal heating
- 11-yr cycle variation
• Ejections and IP disturbances
- Large-scale restructuring
- X-ray plasmoid
- X-ray dimming (vs CME)
- X-ray sigmoid (vs CME)
• Solar flares as magnetic reconnection process
- Soft X-ray loop-with-a-cusp structure, increasing in size with time
- Double-footpoint plus above-a-loop-top hard X-ray sources
- Particle acceleration site in the above-a-loop-top hard X-ray source
- X-ray jets
Flaring Loop and
the Surroundings
* Why do we need study the Sun?
1. “The Sun as a Star” (A Classical Field of Astrophysics)
- Stellar Structure / Evolution
- Dynamo Mechanism (Cosmic Magnetism)
2. Corona: a Prototype for Superhot Astrophysical Plasma
- Why is the corona so hot?
- Coronal Structure / Dynamics
- Sudden Energy Release and Particle Acceleration
* Key Word: Magnetic Reconnection
3. Factors Controlling the Space Weather and Climate
- Solar Wind
- Flares and CMEs as a Cause of IP Disturbances
Science
ISAS / NASA / PPARC / ESA
- Coronal heating
SOLAR-B
- Coronal structure / dynamics
- Elementary processes in Magnetic Reconnection
Launch Date:
Summer 2006
with ISAS M-V-7
Orbit:
Sun synchronous
altitude ~ 600 km
Weight: ~ 900 kg
Mission instruments
- Optical Telescope / Vector Magnetograph (SOT)
- X-ray Telescope (XRT)
- EUV Imaging Spectrometer (EIS)
Structure of the solar atmosphere
SOLAR-B
Lower atmosphere (Photosphere/Chromosphere ) governs the dynamics of
the upper atmosphere (Corona) via magnetic field lines
Key Elements with Solar-B
Instruments
• Solar Optical Telescope (SOT)
Largest optical telescope ever to observe the Sun from space
Diffraction-limited (0.2 – 0.3 arcsec) imaging in 388 – 668 nm
Vector magnetic field measurement at the photosphere
• X-Ray Telescope (XRT)
Highest angular resolution imaging at > 3 MK corona
Wide temperature coverage from below 1 MK to above 10 MK
• EUV Imaging Spectrometer (EIS)
Precise plasma diagnostics in the 17 – 21 nm & 25 – 29 nm ranges
Continuous observation without interruption for 8 months a year
Coordinated observation among the three telescopes
SOT consists of OTA (Optical Telescope Assembly)
and FPP (Focal Plane Package).
Top
door
FPP:
Provided by
NASA/LMSAL
z
y
x
Side
door
Sun
shade
All the telescopes are
complicated. SOT is
just an example.
Details are given
in accompanying
papers.
Shield
tube
Lower
Tube
OTA:
Provided by JAXA/NAO
Mechanical Test Model (2002 May)
OTA
FPP
EIS
OBU
XRT
SOLAR-B
SOLAR-B
Thermal
Test Model
(2002 Oct)
SOT OTA (2004 August)
SOLAR-B
International Collaboration
SOLAR-B
ISAS (Japan): Integration of S/C; Launch & Operation
Mission Instruments:
SOT (optics), XRT (camera), EIS (I/f to S/C)
NASA (US):
SOT (focal plane package), XRT (optics / mech.),
EIS (optics components), NASA polar station(s)
PPARC (UK): EIS (structure, detectors & electronics)
ESA: Polar station(s) for data downlink
Joint Operations and Data Analysis
Data Usage;
Proposal for Observation; etc
SOLAR-B
Solar-B data, together with analysis software
tools, will be opened to the world solar physics
(and related) communities as quickly as possible.
(hopefully in a few months after data acquisition)
We welcome proposals for observation plans
from outside the Solar-B team. (Details TBD)
Collaborative observations with other space- and
ground-based observatories are encouraged.
Any collaborations with, or suggestions/advices
from, theoreticians are most welcome.
Hinotori (1981-1982)
Space Solar Physics
in Japan
Purely Japanese
Yohkoh (1991-2001)
SOLAR-B (2006)
Japan – USA – UK
J – US – UK – ESA (Norway)
Originally prepared for COSPAR 2004
Takeo Kosugi, ISAS/JAXA