| Budget Amount *help |
¥25,610,000 (Direct Cost: ¥19,700,000、Indirect Cost: ¥5,910,000)
Fiscal Year 2013: ¥4,940,000 (Direct Cost: ¥3,800,000、Indirect Cost: ¥1,140,000)
Fiscal Year 2012: ¥4,940,000 (Direct Cost: ¥3,800,000、Indirect Cost: ¥1,140,000)
Fiscal Year 2011: ¥5,070,000 (Direct Cost: ¥3,900,000、Indirect Cost: ¥1,170,000)
Fiscal Year 2010: ¥10,660,000 (Direct Cost: ¥8,200,000、Indirect Cost: ¥2,460,000)
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| Outline of Final Research Achievements |
We have carried out the following two subjects.
(1)By performing high-resolution global 3D magnetohydrodynamical (MHD) simulations for accretion disks, we point out that the temperature structure largely affects the amplification of magnetic field through the distribution of rotation frequency. Even if the ideal MHD approximation is fulfilled, the flow of the mass and the motion of the magnetic flux are different because of turbulent magnetic reconnection.
(2)By MHD simulations for active solar-type stars, we point a global instability associated with the reflection and nonlinear dissipation of Alfven waves. As a result a small change of the energy injection from the photosphere leads to a large change of the stellar wind, and we propose that the mass flux of the solar wind could be as strong as 1000 times of the present value in the past.
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