C134 太陽浮上磁場の 3 次元 MHD シミュレーション
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概要
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It is well known that the solar magnetic fields emerge from the sun's interior of convection zone to the surface as "isolated magnetic flux tubes". However we don't konw where the magnetic fields are formed as the "isolated magnetic flux tubes" in the interior. Therefore in this study is the linear properties of the magnetic buoyancy instability of horizontal magnetic flux sheet situated at the bottom of the convection zone, and then study the nonliner evolution of the instability and resulting formation of the isolated magnetic tube by using a 3-dimensional MHD code.
- 日本流体力学会の論文
- 2001-07-31
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関連論文
- D122 太陽浮上磁場領域の MHD シミュレーション
- D312 太陽大気中の磁気浮力不安定の3次元MHDシミュレーション(D-31 宇宙流体(1),一般講演)
- C134 太陽浮上磁場の 3 次元 MHD シミュレーション