C124 入れ子状格子を用いた星形成のシミュレーション

概要

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We developed a numerical simulation code using a nested grid method. The code allows us to follow a collapse and fragmentation of molecular cloud cores with a fine resolution. Our simulations show that a molecular cloud core, of which size is 0.1 pc, gravitationally collapses to form a opaque core, of which size is 10-100 AU. The core fragments into seeds of binary stars, of which size is 1-10 AU. The fragmentation is classified by the initial perturbations. When the initial cloud has a large perturbation of barmode, the opaque core is elongated enough to fragment into two clumps. When the initial cloud has small perturbation of barmode, a central clump surrounded by spiral arms is formed. The spiral arms fragment into the dense clumps. These clumps are gravitationally bounded, which correspond to seeds of binary stars.
日本流体力学会の論文
2001-07-31