Kes 79中的一个中心致密天体：超临界区和中微子期望
A Central Compact Object in Kes 79: The hypercritical regime and neutrino expectation
摘要：
我们提出了一个强吸积到磁化原中子星的Kesteven 79（Kes 79）方案的磁流体动力学模拟。超新星遗迹Kes 79，用钱德拉ACIS-I仪器观测了大约8.3小时，位于天鹰座，距离银道面7.1千秒差距。这是一个银河系和一个非常年轻的对象，估计年龄为6 kyr。钱德拉的图像首次揭示了遗迹中心的点状源。Kes 79致密残骸属于一类特殊的天体，即所谓的中央致密天体，它没有证据表明周围有脉冲星风星云。在这项工作中，我们表明，淹没的磁场在超临界阶段可以解释这种行为的Kes 79和其他CCO。这种制度的模拟进行了自适应网格细化程序FLASH在两个空间维度，包括中微子的辐射损失和适当的状态方程，这样的制度。根据模拟结果，我们估计在超级神冈实验中预期的热中微子数量为733 $\pm$ 364。此外，我们计算了地球上的祖先模型的风味比。
英文摘要：
We present magnetohydrodynamical simulations of a strong accretion onto magnetized proto-neutron stars for the Kesteven 79 (Kes 79) scenario. The supernova remnant Kes 79, observed with the Chandra ACIS-I instrument during approximately 8.3 h, is located in the constellation Aquila at a distance of 7.1 kpc in the galactic plane. It is a galactic and a very young object with an estimate age of 6 kyr. The Chandra image has revealed, for the first time, a point-like source at the center of the remnant. The Kes 79 compact remnant belongs to a special class of objects, the so-called Central Compact Objects, which exhibits no evidence for a surrounding pulsar wind nebula. In this work we show that the submergence of the magnetic field during the hypercritical phase can explain such behavior for Kes 79 and others CCOs. The simulations of such regime were carried out with the adaptive-mesh-refinement code FLASH in two spatial dimensions, including radiative loss by neutrinos and an adequate equation of state for such regime. From the simulations, we estimate that the number of thermal neutrinos expected on the Hyper-Kamiokande Experiment is 733$\pm$364. In addition, we compute the flavor ratio on Earth for a progenitor model.
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