O型星低质量损失率的独立符号
Independent Signs of Lower Mass-Loss Rates for O-Type Stars
摘要：
我讨论的观测证据-独立的恒星风本身的直接光谱诊断-表明O型星的质量损失率需要向下修正大约三个或更多的因素，符合最近观察到的质量损失率丛生风。这些独立的限制包括在LBV爆发中观测到的大质量损失率，演化的大质量恒星如LBV和WNH星的大质量，在低金属丰度环境中的WR星，在不同金属丰度下观测到的大质量恒星的旋转速率，超新星似乎违背了恒星演化中高质量损失率的预期，以及其他线索。我特别注意的反馈的作用，将导致更高的质量损失率，驾驶恒星爱丁顿极限太特别注意反馈的作用，将导致更高的质量损失率，驾驶恒星的爱丁顿极限太快，因此使更高的速率显得非常难以置信。其中一些论点本身可能有不止一种解释，但它们共同描绘了一幅一致的画面，即O型恒星的稳定线驱动风具有较低的质量损失率，并且显着聚集。
英文摘要：
I discuss observational evidence -- independent of the direct spectral diagnostics of stellar winds themselves -- suggesting that mass-loss rates for O stars need to be revised downward by roughly a factor of three or more, in line with recent observed mass-loss rates for clumped winds. These independent constraints include the large observed mass-loss rates in LBV eruptions, the large masses of evolved massive stars like LBVs and WNH stars, WR stars in lower metallicity environments, observed rotation rates of massive stars at different metallicity, supernovae that seem to defy expectations of high mass-loss rates in stellar evolution, and other clues. I pay particular attention to the role of feedback that would result from higher mass-loss rates, driving the star to the Eddington limit too particular attention to the role of feedback that would result from higher mass-loss rates, driving the star to the Eddington limit too soon, and therefore making higher rates appear highly implausible. Some of these arguments by themselves may have more than one interpretation, but together they paint a consistent picture that steady line-driven winds of O-type stars have lower mass-loss rates and are significantly clumped.
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