Clump mass function at an early stage of molecular cloud evolution - I. A statistical approach

被引：14
作者：
Donkov, Sava [1 ]
Veltchev, Todor V. [2 ,3 ]
Klessen, Ralf S. [3 ]
机构：
[1] Tech Univ, Dept Appl Phys, Sofia 1000, Bulgaria
[2] Univ Sofia, Fac Phys, Sofia 1164, Bulgaria
[3] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-69120 Heidelberg, Germany
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2012年 / 423卷 / 01期
关键词：
turbulence; methods: statistical; ISM: clouds; ISM: structure; PROBABILITY-DISTRIBUTION; TURBULENT FRAGMENTATION; ISOTHERMAL TURBULENCE; INTERSTELLAR CLOUDS; INITIAL CONDITIONS; MAGNETIC-FIELDS; CORES; SPECTRA; ORION; SIMULATIONS;
D O I：
10.1111/j.1365-2966.2012.20939.x
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We derive the mass function of condensations (clumps) which were formed through a turbulent cascade over a range of spatial scales L= 20 pc during early, predominantly turbulent evolution of a molecular cloud. The approach rests upon the assumption of a statistical clump massdensity relationship n?mx with a scale dependence of the exponent x obtained from equipartition relations between various forms of energy of clumps. The derived clump mass function (ClMF) could be represented by series of two or three power laws, depending on the chosen equipartition relation, the velocity scaling index and the type of turbulent forcing. The high-mass ClMF exhibits an average slope G?-1, typical for fractal clouds, whereas its intermediate-mass part is shallower or flattened, in agreement with some observational studies.
引用
收藏
页码：889 / 899
页数：11
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