We study the star formation efficiency per free‐fall time(ϵ_ff) of a self‐gravitating molecular cloud (MC) in the presence of dimensionless thermodynamic efficiency factor ϵ, quantified by taking the ratio of radiation luminosity to the gravitational energy released per free‐fall time (i.e., ) where 0 < ϵ < 1. The results of previous studies indicated that theoretically calculated star formation efficiency of the self‐gravitating MC is larger than the results obtained by observation. These differences may occur due to systematic errors in addition to other physical factors. Currently, there is no single complete model describing star formation efficiency because stars form in a complex and dynamically varying environment. Based on this conceptual framework, we model the equation of star formation efficiency in free‐fall time (ϵ_ff). Moreover, we formulated stellar mass in terms of star formation efficiency by combining the critical mass and the stellar mass models taken from literature. The results indicate that the thermodynamic efficiency factor together with fundamental parameters of the cloud and the time scales play a crucial role in describing the star formation efficiency (SFE) of self‐gravitating MC in its free‐fall time.

中文翻译：

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热力学效率在设定自重分子云的恒星形成效率中的作用

我们研究在存在无量纲热力学效率因子ϵ的情况下，自引力分子云（MC）的每自由下落时间（ϵ _ff）的恒星形成效率，可通过采用辐射光度与每自由释放的重力能量之比来量化下降时间（即），其中0 <ϵ <1。先前的研究结果表明，从理论上计算出的自引力MC的恒星形成效率要大于通过观测获得的结果。这些差异可能是由于除其他物理因素之外的系统错误而发生的。当前，没有单个完整的模型描述恒星形成效率，因为恒星是在复杂且动态变化的环境中形成的。在此概念框架的基础上，我们对自由落体时间（ϵ _ff）中恒星形成效率方程建模）。此外，我们结合临界质量和取自文献的恒星质量模型，根据恒星形成效率制定了恒星质量。结果表明，热力学效率因子以及云的基本参数和时标在描述自重MC自由落体时的恒星形成效率（SFE）方面起着至关重要的作用。