论文标题
群众损失和爱丁顿参数：一种新的巨大恒星的质量损失配方
Mass loss and the Eddington parameter: a new mass-loss recipe for hot and massive stars
论文作者
论文摘要
通过恒星风的质量损失在巨大恒星的进化中起主要作用。尤其是非常巨大的恒星（VMS，$> 100 \，m _ {\ odot} $）的质量损失率是高度不确定的。这样的恒星在主序列上展示了狼射线光谱形态（WNH）。金属贫困的VMS是伽马射线爆发和配对超新星的祖细胞。在这项研究中，我们将Castor，Abbott＆Klein广泛使用的恒星风理论从光学薄（O Star）扩展到光学厚的主序列（WNH）风状态。特别是，我们以一种能够解释对Eddington参数的经验质量差异依赖性（$γ_{\ rm E} $）的方式修改质量损失率公式。新的质量损失配方适合将恒星和非常巨大的恒星纳入当前的恒星进化模型。它做出了可验证的预测，即如何用金属性和爱丁顿参数的质量量表尺度尺度，从光学薄的O恒星到光学厚的WNH恒星风发生过渡。 In the case of the star cluster R136 in the Large Magellanic Cloud we find in the optically thin wind regime $\dot{M} \propto Γ_{\rm e}^{3}$ while in the optically thick wind regime $\dot{M} \propto 1/ (1 - Γ_{\rm e})^{3.5}$.从光学薄到光学厚的风的过渡发生在$γ_ {\ rm e，trans} \大约0.47 $。过渡质量降低速率为$ \ log \ dot {m}〜（m _ {\ odot} \ mathrm {yr}^{ - 1}）\ ofty-oft-of-of-of vink＆gräfener的预测属于$ f _ _ _ _ _ _ { 0.23 _ { - 0.15}^{+0.40} $。
Mass loss through stellar winds plays a dominant role in the evolution of massive stars. In particular the mass-loss rates of very massive stars (VMSs, $> 100\,M_{\odot}$) are highly uncertain. Such stars display Wolf-Rayet spectral morphologies (WNh) whilst on the main-sequence. Metal-poor VMSs are progenitors of gamma-ray bursts and pair instability supernovae. In this study we extended the widely used stellar wind theory by Castor, Abbott & Klein from the optically thin (O star) to the optically thick main-sequence (WNh) wind regime. In particular we modify the mass-loss rate formula in a way that we are able to explain the empirical mass-loss dependence on the Eddington parameter ($Γ_{\rm e}$). The new mass-loss recipe is suitable for incorporation into current stellar evolution models for massive and very massive stars. It makes verifiable predictions, namely how the mass-loss rate scales with metallicity and at which Eddington parameter the transition from optically thin O star to optically thick WNh star winds occurs. In the case of the star cluster R136 in the Large Magellanic Cloud we find in the optically thin wind regime $\dot{M} \propto Γ_{\rm e}^{3}$ while in the optically thick wind regime $\dot{M} \propto 1/ (1 - Γ_{\rm e})^{3.5}$. The transition from optically thin to optically thick winds occurs at $Γ_{\rm e, trans} \approx 0.47$. The transition mass-loss rate is $\log \dot{M}~(M_{\odot} \mathrm{yr}^{-1}) \approx -4.76 \pm 0.18$, which is in line with the prediction by Vink & Gräfener assuming a volume filling factor of $f_{\rm V} = 0.23_{-0.15}^{+0.40}$.
