Generation of density inhomogeneities by magnetohydrodynamic waves in two dimensions
arXiv:astro-ph/0605258 · doi:10.1111/j.1365-2966.2006.10524.x
Abstract
Using two dimensional simulations, we study the formation of structures with a high-density contrast by magnetohydrodynamic waves in regions in which the ratio of thermal to magnetic pressure is small. The initial state is a uniform background perturbed by fast-mode wave. Our most significant result is that dense structures persist for far longer in a two-dimensional simulation than in the one-dimensional case. Once formed, these structures persist as long as the fast-mode amplitude remains high.
6 pages, 7 figures, accepted by MNRAS
References in corpus (7)
- The Stellar IMF from Turbulent Fragmentation
- The Physics of Star Formation
- Physical vs. Observational Properties of Clouds in Turbulent Molecular Cloud Models
- The Lifetimes and Evolution of Molecular Cloud Cores
- The Formation of Self-Gravitating Cores in Turbulent Magnetized Clouds
- Quiescent Cores and the Efficiency of Turbulence-Accelerated, Magnetically Regulated Star Formation
- Analysis of Clumps in Molecular Cloud Models: Mass Spectrum, Shapes, Alignment and Rotation
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