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Paper: Star Formation in a Turbulent Cloud Core with Self-gravitational MHD Adaptive Mesh Refinement
Volume: 429, Numerical Modeling of Space Plasma Flows, Astronum-2009
Page: 22
Authors: Matsumoto, T.
Abstract: Protostellar collapse of a turbulent magnetized cloud core is investigated by using a new adaptive mesh refinement (AMR) code, SFUMATO. The AMR code solves self-gravitational magnetohydrodynamics (MHD) problems, achieving the second-order accuracy in space and time. For a model of a cloud core, a spherical cloud with an uniform magnetic field and turbulent velocity is considered at the initial stage. The cloud is moderately massive; Eth/|Egrav| = 0.5, where Eth and Egrav denote thermal and gravitational energies, respectively. The turbulence with a higher Mach number produces larger perturbation in the low density region, although the collapsing dense region exhibit an axisymmetric disk oriented perpendicular to the local magnetic field. All the models with the initial Mach numbers ranging from 0.5 to 5 do not exhibit fragmentation.
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