Max-Planck-Institut für Physik (Werner-Heisenberg-Institut), Föhringer Ring 6, 80805 München, Germany.
Phys Rev Lett. 2013 Sep 20;111(12):121104. doi: 10.1103/PhysRevLett.111.121104. Epub 2013 Sep 18.
The first full-scale three-dimensional core-collapse supernova (SN) simulations with sophisticated neutrino transport show pronounced effects of the standing accretion shock instability (SASI) for two high-mass progenitors (20 and 27 M([Symbol: see text])). In a low-mass progenitor (11.2 M([Symbol: see text])), large-scale convection is the dominant nonradial hydrodynamic instability in the postshock accretion layer. The SASI-associated modulation of the neutrino signal (80 Hz in our two examples) will be clearly detectable in IceCube or the future Hyper-Kamiokande detector, depending on progenitor properties, distance, and observer location relative to the main SASI sloshing direction. The neutrino signal from the next galactic SN can, therefore, diagnose the nature of the hydrodynamic instability.
首次利用精细的中微子输运模型进行的全尺寸三维核心塌缩超新星（SN）模拟显示，在两个高质量前身星（20 和 27 M([Symbol: see text]））中，静止吸积激波不稳定性（SASI）具有显著影响。在一个低质量前身星（11.2 M([Symbol: see text]））中，在激波后吸积层中，大规模对流是主要的非径向流体动力学不稳定性。在我们的两个例子中，SASI 相关的中微子信号调制（80 Hz）将在 IceCube 或未来的 Hyper-Kamiokande 探测器中清晰可检测，具体取决于前身星性质、距离以及观测者相对于主要 SASI 晃动方向的位置。因此，下一个星系 SN 的中微子信号可以诊断流体动力学不稳定性的性质。
