利用内对流层为抖动射流爆炸机理提供angular momentum
Supplying angular momentum to the jittering jets explosion mechanism using inner convection layers
摘要：
我们进行一维恒星演化模拟的质量范围$13-20 M_{\odot}$晚核心崩溃的时间，发现一个内部强对流区与大的特定角动量波动出现在崩溃期间的铁核心的边缘。在坍缩过程中，这一区域的压缩增加了那里的光度和对流速度，使得特定的角动量波动在j_{conv} ~ 5 × 10 ^15 cm ^2/sec的量级。如果我们考虑到三维模拟显示的对流速度比混合长度理论给出的速度大三到四倍，并且在半径约100 km的失速激波的激波后区域中的螺旋形静止吸积激波不稳定性放大了扰动，我们的结论是，在核心崩溃期间发展的波动很可能导致随机（间歇性的）围绕新生中子星的吸积盘。在得出这一结论时，我们还提出了两个基本假设，我们讨论的不确定性。这种间歇性的圆盘可以发射出喷射流，在抖动的喷射流爆炸机制的框架内爆炸恒星。
英文摘要：
We conduct one-dimensional stellar evolution simulations in the mass range $13-20 M_{\odot}$ to late core collapse times and find that an inner vigorous convective zone with large specific angular momentum fluctuations appears at the edge of the iron core during the collapse. The compression of this zone during the collapse increases the luminosity there and the convective velocities, such that the specific angular momentum fluctuations are of the order of j_{conv}~5x10^15cm^2/sec. If we consider that three-dimensional simulations show convective velocities that are three to four times larger than what the mixing length theory gives, and that the spiral standing accretion shock instability in the post-shock region of the stalled shock at a radius of ~100km amplify perturbations, we conclude that the fluctuations that develop during core collapse are likely to lead to stochastic (intermittent) accretion disks around the newly born neutron star. In reaching this conclusion we also make two basic assumptions with uncertainties that we discuss. Such intermittent disks can launch jets that explode the star in the frame of the jittering jets explosion mechanism.
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