Quasi-periodic oscillations inferred during rare magnetar giant flare tails were initially interpreted as torsional oscillations of the neutron star (NS) crust, and have been more recently described as global core+crust perturbations. Similar frequencies are also present in high-signal-to-noise magnetar short bursts. In magnetars, disturbances of the field are strongly coupled to the NS crust regardless of the triggering mechanism of short bursts. For low-altitude magnetospheric magnetar models of fast radio bursts (FRBs) associated with magnetar short bursts, such as the low-twist model, crustal oscillations may be associated with additional radio bursts in the encompassing short burst event (as recently suggested for SGR 1935+2154). Given the large extragalactic volume probed by wide-field radio transient facilities, this offers the prospect of studying NS crusts leveraging samples far more numerous than galactic high-energy magnetar bursts by studying statistics of subburst structure or clustered trains of FRBs. We explore the prospects for distinguishing NS equation of state models with increasingly larger future sets of FRB observations. Lower l-number eigenmodes (corresponding to FRB time intervals of ∼5–50 ms) are likely less susceptible than high-l modes to confusion by systematic effects associated with the NS crust physics, magnetic field, and damping. They may be more promising in their utility, and also may corroborate models where FRBs arise from mature magnetars. Future observational characterization of such signals can also determine whether they can be employed as cosmological “standard oscillators” to constrain redshift, or can be used to constrain the mass of FRB-producing magnetars when reliable redshifts are available.

在罕见的磁星巨耀斑尾部推断的准周期振荡最初被解释为中子星 (NS) 地壳的扭转振荡，最近被描述为全球核心 + 地壳扰动。类似的频率也存在于高信噪比的磁星短脉冲中。在磁星中，无论短暴的触发机制如何，磁场扰动都与 NS 地壳强烈耦合。对于与磁星短爆发相关的快速无线电爆发 (FRB) 的低空磁层磁星模型，例如低扭曲模型，地壳振荡可能与包含的短爆发事件中的额外无线电爆发有关（如最近建议的 SGR 1935 +2154）。鉴于广域无线电瞬变设施探测到的巨大河外体积，这为利用比银河系高能磁星爆发更多的样本来研究 NS 地壳提供了前景，即通过研究亚爆结构或 FRB 集群序列的统计数据。我们探索了用越来越大的未来 FRB 观测集区分 NS 状态模型方程的前景。降低l 数本征模式（对应于约 5-50 ms 的 FRB 时间间隔）可能比高l模式更不容易被与 NS 地壳物理、磁场和阻尼相关的系统效应混淆。它们在效用方面可能更有前景，并且也可能证实成熟磁星产生 FRB 的模型。未来对此类信号的观测表征还可以确定它们是否可以用作宇宙学“标准振荡器”来限制红移，或者在可靠的红移可用时可以用来限制产生 FRB 的磁星的质量。