Repeating fast radio bursts from collapses of the crust of a strange star.
Repeating fast radio bursts from collapses of the crust of a strange star.
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一颗奇怪恒星的地壳塌陷重复产生快速射电爆发
DOI：
10.1016/j.xinn.2021.100152
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发表时间：
2021-11-28
期刊：
影响因子：
--
通讯作者：
Huang Y
中科院分区：
文献类型：
--
作者：
Geng J;Li B;Huang Y
奇异星（SS）是由去束缚夸克组成的致密物体。由于可能存在由正常强子物质组成的薄壳，并使SS的整个表面模糊不清，因此很难将SS与中子星区分开来。在这里，我们认为，有趣的重复快速射电爆发（FRB）产生的间歇性分数崩溃的地壳的SS引起的再填充的物质从其低质量的同伴。在我们的场景中，可以很好地理解FRB的周期性/零星/集群的时间行为。特别是，周期性归因于通过盘不稳定性的吸积率的调制。为了解释180916.J0158+65的重复FRB源的~16天周期性，我们调用了一个粘性参数为0.004、吸积速率为3 × 1016 g s−1的沙库拉-苏亚耶夫盘。如果我们的假设被未来的观测所支持，将成为奇异夸克物质假说的间接证据。奇异夸克星是由u、d和s夸克组成的极其致密的天体。奇异夸克星星壳的部分坍缩可以解释FRB 180916的重复现象。从伴星星星吸积的物质在极区积累并触发局部坍缩。FRB 180916的16天周期源于吸积盘的热粘性不稳定性，并且活动窗口对应于系统的高吸积状态
Strange stars (SSs) are compact objects made of deconfined quarks. It is hard to distinguish SSs from neutron stars as a thin crust composed of normal hadronic matter may exist and obscure the whole surface of the SS. Here we suggest that the intriguing repeating fast radio bursts (FRBs) are produced by the intermittent fractional collapses of the crust of an SS induced by refilling of materials accreted from its low-mass companion. The periodic/sporadic/clustered temporal behaviors of FRBs could be well understood in our scenario. Especially, the periodicity is attributed to the modulation of accretion rate through the disk instabilities. To account for a ~16-day periodicity of the repeating FRB source of 180916.J0158+65, a Shakura-Sunyaev disk with a viscosity parameter of 0.004 and an accretion rate of 3 × 1016 g s−1 is invoked. Our scenario, if favored by future observations, will serve as indirect evidence for the strange quark matter hypothesis. Strange quark stars are extremely compact objects mainly composed of u, d, and s quarks Fractional collapse of the crust of a strange quark star can explain the repeating FRB 180916 Materials accreted from the companion star accumulate at the polar region and trigger the local collapse The 16-day periodicity of FRB 180916 originates from the thermal-viscous instability of the accretion disk, and the active window corresponds to a high accretion state of the system
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