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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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