Tidal resonances in the final seconds of a binary neutron-star inspiral can excite oscillation modes in one or both of the constituents to large amplitudes. Under favorable circumstances, resonant pulsations can overstrain the stellar crust and unleash a torrent of magnetoelastic energy that manifests as a gamma-ray “precursor flare.” We show that for realistic, stratified stars rotating with a spin frequency of $\gtrsim 30\mathrm{Hz}$, the fundamental $g$ mode or its first overtone can also execute a differential rotation in the crust such that a magnetic field of strength $\gtrsim {10}^{13}\mathrm{G}$ is generated via magnetorotational instabilities. This may help to explain observed precursor rates and their luminosities. Premerger magnetic growth would also provide seed magnetic energy for the postmerger remnant.

中文翻译：

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通过共振引起的磁旋转不稳定性实现并合前中子星的磁放大

双中子星螺旋的最后几秒的潮汐共振可以激发一个或两个成分的振荡模式达到大振幅。在有利的情况下，共振脉动会使恒星地壳过度紧张，并释放出磁弹性能量的洪流，表现为伽马射线“前体耀斑”。我们证明，对于以自旋频率旋转的现实​​分层恒星$\gtrsim 30\mathrm{赫兹}$，基本的$G$模式或其第一泛音也可以在地壳中执行微分旋转，使得强度磁场$\gtrsim {10}^{13}\mathrm{G}$是通过磁旋转不稳定性产生的。这可能有助于解释观察到的前体速率及其光度。合并前的磁生长也将为合并后的残余物提供种子磁能。