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arXiv 0709.0202astro-ph
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超大质量恒星能避免双星不稳定性超新星吗？

Can very massive stars avoid Pair-instability Supernovae?

S. Ekström, G. Meynet, A. Maeder

备注：
to be published in the conference proceedings of First Stars III, Santa Fe, 2007
发表信息：
AIPConf.Proc.990:220-224,2008
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摘要：

超大质量的原始恒星（$140 M_{\odot} < M < 260 M_{\odot}$）被认为是以不稳定超新星的形式结束生命的。这样的事件可以通过低金属量恒星中的典型化学特征来追踪，但目前，我们能够观察到的极端贫金属恒星中缺乏这种特征。这是否意味着那些非常巨大的物体并没有形成，与原始恒星形成的情况相反？他们能避免这种悲惨的命运吗？我们探讨了旋转，各向异性质量损失和磁场对一个非常大的人口III模型的核心尺寸的影响，以检查其质量是否被充分修改，以防止对不稳定性。我们得到了一个包含风的各向异性和Tayler-Spruit发电机的$150 M_{\odot}$的第三类模式，其中计算的$\upsilon/\upsilon_{\rm crit}=0.56$避免了对不稳定性爆炸。

英文摘要：

Very massive primordial stars ($140 M_{\odot} < M < 260 M_{\odot}$) are supposed to end their lives as pair-instability supernovae. Such an event can be traced by a typical chemical signature in low metallicity stars, but at the present time, this signature is lacking in the extremely metal-poor stars we are able to observe. Does it mean that those very massive objects did not form, contrarily to the primordial star formation scenarios? Could they avoid this tragical fate? We explore the effects of rotation, anisotropic mass loss and magnetic fields on the core size of a very massive Population III model, in order to check if its mass is sufficiently modified to prevent the pair instability. We obtain that a Population III model of $150 M_{\odot}$ with $\upsilon/\upsilon_{\rm crit}=0.56$ computed with the inclusion of wind anisotropy and Tayler-Spruit dynamo avoids the pair instability explosion.

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