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首页> 外文期刊>The Astrophysical Journal. Letters >A SUPER-EDDINGTON WIND SCENARIO FOR THE PROGENITORS OF TYPE Ia SUPERNOVAE
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A SUPER-EDDINGTON WIND SCENARIO FOR THE PROGENITORS OF TYPE Ia SUPERNOVAE

机译：Ia型超新星前体的超爱丁顿风场

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摘要

The accretion of hydrogen-rich material on to carbon-oxygen white dwarfs (COWDs) is crucial for understanding Type Ia supernova (SN Ia) from the single-degeneratemodel, but this process has not been well understood due to the numerical difficulties in treating H and He flashes during the accretion. For CO WD masses from 0.5 to 1.378 M_⊙ and accretion rates in the range from 10~(?8) to 10~(?5)M_⊙ yr~(?1), we simulated the accretion of solar-composition material on to CO WDs using the state-of-the-art stellar evolution code of MESA. For comparison with steady-state models, we first ignored the contribution from nuclear burning to the luminosity when determining the Eddington accretion rate, and found that the properties of H burning in our accreting CO WD models are similar to those from the steady-state models, except that the critical accretion rates at which the WDs turn into red giants or H-shell flashes occur on their surfaces are slightly higher than those from the steady-state models. However, the super-Eddington wind is triggered at much lower accretion rates than previously thought, when the contribution of nuclear burning to the total luminosity is included. This super-Eddington wind naturally prevents the CO WDs with high accretion rates from becoming red giants, thus presenting an alternative to the optically thick wind proposed by Hachisu et al. Furthermore, the super-Eddington wind works in low-metallicity environments, which may explain SNe Ia observed at high redshifts.
机译：富氢物质在碳氧白矮星（COWD）上的积聚对于从单一简并模型了解Ia型超新星（SN Ia）至关重要，但是由于处理H的数值困难，这一过程尚未得到很好的理解。吸血期间祂闪烁。对于CO WD质量从0.5到1.378M_⊙且吸积率在10〜（？8）到10〜（？5）M_⊙yr〜（？1）范围内，我们模拟了太阳能合成材料在CO WD使用MESA的最新恒星演化代码。为了与稳态模型进行比较，我们在确定爱丁顿积聚率时首先忽略了核燃烧对光度的贡献，发现在我们积聚的CO WD模型中H燃烧的性质与稳态模型相似，除了WD变成红色巨人或H​​形壳闪动的临界吸积率略高于稳态模型。但是，当包括核燃烧对总光度的贡献时，超级爱丁顿风以比以前认为的低得多的吸积率触发。这种超级爱丁顿风自然地阻止了高积聚速率的CO WD变成红色巨人，因此是Hachisu等人提出的光学厚风的替代方案。此外，超级爱丁顿风在低金属环境下工作，这可能解释了在高红移下观测到的SNe Ia。

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