论文标题
恒星辐射反馈在设置恒星质量谱系中的作用是什么？
What is the role of stellar radiative feedback in setting the stellar mass spectrum?
论文作者
论文摘要
尽管经过数十年的理论努力，但仍有辩论恒星初始质量功能（IMF）的物理起源。特别至关重要的是什么设定了分布的峰值。为了调查这个问题，我们使用辐射反馈探索的高分辨率数值模拟，特别是恒星和增生发光性的作用。我们还使用简单的状态方程（EOS）进行模拟，并研究了1000个太阳质量团块，其初始半径分别为0.1和0.4 PC。我们发现，大多数运行均具有辐射转移或EOS，呈现出相似的质谱，其峰值位于0.3-0.5 m $ _ \ odot $和较高质量的PowerLaw样质量分布。但是，当考虑到积聚的发光度时，最紧凑的团块的质谱往往是最高的。对于不太紧凑的效果仍然有限，总体上保持冷。我们的结果支持这样的想法：这是从等温度向绝热状态的过渡，而不是辐射性恒星反馈，该转变的气体密度约为10 $^{10} $ CM $ $^{ - 3} $，负责设置初始质量功能的峰值。这是因为$ i）$ $非常紧凑的团块对此产生的亮度产生重大影响非常罕见，而$ ii）$，因为亮度问题，这表明有效的积聚光度可能弱于预期。
In spite of decades of theoretical efforts, the physical origin of the stellar initial mass function (IMF) is still debated. Particularly crucial is the question of what sets the peak of the distribution. To investigate this issue we perform high resolution numerical simulations with radiative feedback exploring in particular the role of the stellar and accretion luminosities. We also perform simulations with a simple effective equation of state (eos) and we investigate 1000 solar mass clumps having respectively 0.1 and 0.4 pc of initial radii. We found that most runs, both with radiative transfer or an eos, present similar mass spectra with a peak broadly located around 0.3-0.5 M$_\odot$ and a powerlaw-like mass distribution at higher masses. However, when accretion luminosity is accounted for, the resulting mass spectrum of the most compact clump tends to be moderately top-heavy. The effect remains limited for the less compact one, which overall remains colder. Our results support the idea that rather than the radiative stellar feedback, this is the transition from the isothermal to the adiabatic regime, which occurs at a gas density of about 10$^{10}$ cm$^{-3}$, that is responsible for setting the peak of the initial mass function. This stems for the fact that $i)$ extremely compact clumps for which the accretion luminosity has a significant influence are very rare and $ii)$ because of the luminosity problem, which indicates that the effective accretion luminosity is likely weaker than expected.
