The thermodynamics of molecular cloud fragmentation
نویسندگان
چکیده
منابع مشابه
In Situ Formation of Sgra Stars via Disk Fragmentation: Parent Cloud Properties and Thermodynamics
The formation of the massive young stars surrounding SgrA* is still an open question. In this paper, we simulate the infall of a turbulent molecular cloud toward the Galactic Center (GC). We adopt two different cloud masses (4.3 × 104 M sun and 1.3 × 105 M sun). We run five simulations: the gas is assumed to be isothermal in four runs, whereas radiative cooling is included in the fifth run. In ...
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The fragmentation of molecular cloud cores a factor of 1.1 denser than the critical Bonnor-Ebert sphere is examined though three-dimensional numerical simulations. A nested grid is employed to resolve fine structure down to 1 AU while following the entire structure of the molecular cloud core of radius 0.14 pc. A barotropic equation of state is assumed to take account of the change in temperatu...
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Recent calculations with a two-fluid smoothed particle hydrodynamics (SPH) code of the collapse of a magnetized dense core have found little evidence for fragmentation. These calculations have been interpreted as implying that magnetic braking by magnetic tension forces is sufficient to inhibit fragmentation, contrary to a suggestion by Boss that magnetic fields might encourage fragmentation. H...
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Context. Observations suggest that low-mass stars condense out of dense, relatively isolated, molecular cloud cores, with each core spawning a small-N cluster of stars. Aims. Our aim is to identify the physical processes shaping the collapse and fragmentation of a 5.4 M⊙ core, and to understand how these processes influence the mass distribution, kinematics, and binary statistics of the resulti...
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Observations of stars in the vicinity of the Sun show that binary systems are prevalent and appear to be a general outcome of the star-formation process. One of the major goals of this research is to understand the nature of the formation of binary and multiple stellar systems with typical low-mass stars (∼ 0.2 to 3 M ) and the physical properties of these systems. Basic questions concerning th...
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ژورنال
عنوان ژورنال: Astronomy and Astrophysics
سال: 2010
ISSN: 0004-6361,1432-0746
DOI: 10.1051/0004-6361/200912236