Clump mass function at an early stage of molecular cloud evolution – II. Galactic cloud complexes
Clump mass function at an early stage of molecular cloud evolution – II. Galactic cloud complexes
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分子云演化早期阶段的团块质量函数 – II。
DOI：
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
R. Klessen
中科院分区：
文献类型：
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作者：
T. Veltchev;S. Donkov;R. Klessen
通过与不同作者从银河系云复合体的分子发射和尘埃连续谱图中得到的团块质量分布进行比较，对Donkov，Veltchev和Klessence开发的用于推导团块质量函数（ClMF）的统计方法进行了观测测试。结果表明，占主导地位的集团人口的引力有界性，考虑或不考虑其热能和磁能的贡献。ClMF可以由两个幂律函数的组合来表示，这两个幂律函数被大约10到100个太阳质量的特征质量分开。中等质量的ClMF的斜率很浅，几乎是恒定的（-0.25 \gtrsim \Gamma_{IM} \gtrsim -0.55），而高质量部分由暗示重力不稳定团块并在更宽范围内显示斜率的模型拟合（-0.9 \gtrsim \Gamma_{IM} \gtrsim -1.6），以恒星初始质量函数（\Gamma_{HM} \gtreqless -1.3）为中心。
The statistical approach for derivation of the clump mass function (ClMF) developed by Donkov, Veltchev & Klessen is put to observational test through comparison with mass distributions of clumps from molecular emission and dust continuum maps of Galactic cloud complexes, obtained by various authors. The results indicate gravitational boundedness of the dominant clump population, with or without taking into account the contribution of their thermal and magnetic energy. The ClMF can be presented by combination of two power-law functions separated by a characteristic mass from about ten to hundreds solar masses. The slope of the intermediate-mass ClMF is shallow and nearly constant (-0.25 \gtrsim \Gamma_{IM} \gtrsim -0.55) while the high-mass part is fitted by models that imply gravitationally unstable clumps and exhibit slopes in a broader range (-0.9 \gtrsim \Gamma_{IM} \gtrsim -1.6), centered at the value of the stellar initial mass function (\Gamma_{HM} \gtreqless -1.3).