Related Progenitor Models for Long-duration Gamma-Ray Bursts and Type Ic Superluminous Supernovae
Related Progenitor Models for Long-duration Gamma-Ray Bursts and Type Ic Superluminous Supernovae
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DOI：
10.3847/1538-4357/aabfc1
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发表时间：
2018-04
期刊：
影响因子：
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通讯作者：
D. R. Aguilera-Dena;N. Langer;T. Moriya;A. Schootemeijer
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作者：
D. R. Aguilera-Dena;N. Langer;T. Moriya;A. Schootemeijer
我们模拟了快速旋转的沃尔夫-拉叶星在质量范围为5 M-100 M-100 M-100 M的后期演化和质量损失历史。我们发现，准化学均匀演化的单星计算增强混合保留很少或没有氦，并与Ic型超新星兼容。在我们的低质量模型中，更有效地去除核心角动量和预期的更小的紧凑物体质量，导致核心自旋在磁星驱动的超亮超新星所建议的范围内。我们的高质量模型保留了较大的特定核心角动量，预计长持续时间的伽马射线爆发的Bracksar的情况。由于没有明显的氦包层，核心氦耗尽后迅速增加的中微子发射导致整个星星加速收缩，导致强烈的自旋和离心驱动的质量损失，在核心坍塌前的最后几年到几十年的速度高达。由于我们的低质量模型中的角动量输运增强了包络自旋，因此它们显示出最大的离心强制质量损失相对量，即，达到预期喷出物质量的25%我们最大的质量模型演化到脉动对不稳定状态。因此，我们可以预期，对于喷发物质量低于1000万吨的Ic型超亮超新星，以及喷发物质量高于3000万吨的最大质量的发动机驱动爆炸，都有与富含C/O的星周介质相互作用的特征。这种相互作用的迹象应该在超新星爆发的早期就可以观察到;它们可能与在超亮超新星的光变曲线中观察到的隆起有关，或者与Ic型超亮超新星Gaia 16 apd的大质量星周CO壳层有关。
We model the late evolution and mass loss history of rapidly rotating Wolf–Rayet stars in the mass range 5 M⊙…100 M⊙). We find that quasi-chemically homogeneously evolving single stars computed with enhanced mixing retain very little or no helium and are compatible with Type Ic supernovae. The more efficient removal of core angular momentum and the expected smaller compact object mass in our lower-mass models lead to core spins in the range suggested for magnetar-driven superluminous supernovae. Our higher-mass models retain larger specific core angular momenta, expected for long-duration gamma-ray bursts in the collapsar scenario. Due to the absence of a significant He envelope, the rapidly increasing neutrino emission after core helium exhaustion leads to an accelerated contraction of the whole star, inducing a strong spin-up and centrifugally driven mass loss at rates of up to in the last years to decades before core collapse. Because the angular momentum transport in our lower-mass models enhances the envelope spin-up, they show the largest relative amounts of centrifugally enforced mass loss, i.e., up to 25% of the expected ejecta mass. Our most massive models evolve into the pulsational pair-instability regime. We would thus expect signatures of interaction with a C/O-rich circumstellar medium for Type Ic superluminous supernovae with ejecta masses below ∼10 M⊙ as well as for the most massive engine-driven explosions with ejecta masses above ∼30 M⊙. Signs of such interaction should be observable at early epochs of the supernova explosion; they may be related to bumps observed in the light curves of superluminous supernovae, or to the massive circumstellar CO-shell proposed for Type Ic superluminous supernova Gaia16apd.