A Magnetohydrodynamic Simulation of the Interaction between the Solar Wind and Comet Halley

太阳风与哈雷彗星相互作用的磁流体动力学模拟

• 批准号: 61540306
• 负责人: OGINO Tatsuki
• 金额: $ 1.09万
• 依托单位: Research Institute of Atmospherics, Nagoya University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (C)
• 财政年份: 1986
• 资助国家: 日本
• 起止时间: 1986 至 1987
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-61540306/
• 关键词: Comet Halley; Solar wind; Interaction; Magnetohydrodynamics; 計算機シミュレーション; シミュレーション

The interaction between the solar wind and the plasmas produced form cometary gases has been modeled by using a three-dimensional time-dependent magneto-hydrodynamic (MHD) simulation with the cometary mass loading. The model reproduced several features observed by the recent missions to comet Halley.A weak bow shock was located 3.2x10^5 km in front of the comet. The magnetic field increased by a factor of 3.7 across this weak bow shock and continued to increase up to the contact surface (B_<max>/B_<IMF>= 6-8). The plasma temperature increased across the bow shock and decreased nearer to the comet. Interplanetary magnetic field (IMF) lines were hung up on the comet and formed a long plasma tail in which the lobe field was quite strong and B_<lobe>/B_<IMF>-5. A cold dense plasma sheet formed in the tail and this thin plasma sheet was oriented normal the IMF direction.Ray-like structure and a plasmoid with high plasma pressure are formed in thecometary plasma tail and propagate tailward with a local Alfven speed, when the dynamic pressure of solar wind or the IMF changes. These results give an explanation on the dynamics of cometary tail which were shown by the observationsusing a lot of photos. Our global MHD simulation in the solar wind-comet interaction has made clear the role of cometary mass loading and also has given animportant incitement in comparison with the interaction between the solar wind and other planets.

太阳风与等离子体产生的彗星气体之间的相互作用是通过使用彗星质量负载的三维时间依赖性磁动力学（MHD）模拟来建模的。该模型重现了最近的任务对Halley彗星观察到的几个功能。弱的弓形冲击位于彗星前面3.2x10^5 km。在这种弱的弓形冲击中，磁场增加了3.7倍，并继续增加到接触表面（B_ <max>/b_ <imf> = 6-8）。在整个弓形冲击中，血浆温度升高，并靠近彗星。星际磁场（IMF）线悬挂在彗星上，形成一个长的等离子体尾巴，其中叶片场很强，b_ <lobe>/b_ <imf> -5。在尾部形成的冷致密的等离子体表和该薄的等离子表的定向正常。IMF方向。类似于射线的结构和高血浆压力的等离子体在thecometary血浆尾部形成，当Solar风的动态压力或IMF变化时，在局部等离子体的尾部中以局部的Alfven速度传播尾巴。这些结果可以解释彗星尾巴的动态，这是通过观察到很多照片所显示的。我们在太阳能风频率相互作用中的全球MHD模拟已经明确了彗星质量负载的作用，并且与太阳风与其他行星之间的相互作用相比，也给出了动画煽动。

项目成果

T.Ogino: UCLA IGPP Publ. 3047 submitted to Journal of Geophysical Research. (1987)

T.Ogino：加州大学洛杉矶分校 IGPP 出版物。

T.Ogino: The International Plasma Workshop in Tokyo,ed.by H.Kikuchi,Springer. (1988)

T.Ogino：东京国际等离子体研讨会，H.Kikuchi 编辑，Springer。

T. Ogino: "A three dimensional MHD simulation of the interaction of the solar wind with comet Halley" UCLA IGPP Publ. 3047 submitted to Journal of Geophysical Research. (1987)

T. Ogino：“太阳风与哈雷彗星相互作用的三维 MHD 模拟”加州大学洛杉矶分校 IGPP 出版物。

T. Ogino: "Two dimensional MHD simulation of the interaction between the solar wind and cometary outflowing plasmas" ISAS Research Report. 15. 109-120 (1986)

T. Ogino：“太阳风与彗星流出等离子体之间相互作用的二维 MHD 模拟”ISAS 研究报告。

T.Ogino: Proceedings of Chapman Conference on Plasma Waves and Instabilities in Magnetospheres and at Comets,by conveners:H.Oya and B.T.Tsurutani,. 84-87 (1987)

T.Ogino：查普曼关于磁层和彗星中的等离子体波和不稳定性的会议记录，召集人：H.Oya 和 B.T.Tsurutani。