Multimessenger emission from tidal waves in neutron star oceans
Multimessenger emission from tidal waves in neutron star oceans
复制标题
中子星海洋中潮汐波的多信使发射
DOI：
10.1093/mnras/stad389
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发表时间：
2023
影响因子：
4.8
通讯作者：
Márka, Szabolcs
中科院分区：
文献类型：
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作者：
Sullivan, Andrew G.;Alves, Lucas M. B.;Spence, Georgina O.;Leite, Isabella P.;Veske, Doğa;Bartos, Imre;Márka, Zsuzsa;Márka, Szabolcs
天体物理学双星系统中的中子星是多信使天体物理学令人兴奋的来源。致密双星系统电磁瞬变的一个潜在来源是中子星星海洋，即包裹中子星星的外部流体层。本文对中子星星海洋中的潮汐波及其后果进行了初步研究。具体来说，我们调查如何在中子星星海洋振荡模式可以在紧凑的双螺旋和抛物面遇到潮汐激发。我们发现，中子星星海洋可以维持频率在0.01和20赫兹之间的潮汐波。我们的研究结果表明，潮汐共振中子星星海浪可能作为一个从未研究过的源前体电磁辐射中子星黑洞和双中子星星合并。如果伴随着电磁耀斑，潮汐共振中子星星海浪，其能量预算可达1046尔格，可以作为早期预警信号（合并前101分钟）的紧凑的双合并。同样，激发的海洋潮汐波将与中子星星抛物面相遇相吻合。根据中子星星海洋模型和耀斑发射的假设，潮汐共振的海洋耀斑可以被费米核光谱望远镜阵列（努斯塔）探测到，探测率高达100 Mpc，中子星双星的探测率高达10.7 yr− 1，中子星-黑洞双星的探测率高达10.6 yr− 1。观测中子星星海洋潮汐波沿着引力波的辐射，将有助于深入了解中子星星表面的状态方程、中子星星海洋和地壳的组成以及中子星星物理学。
Neutron stars in astrophysical binary systems represent exciting sources for multimessenger astrophysics. A potential source of electromagnetic transients from compact binary systems is the neutron star ocean, the external fluid layer encasing a neutron star. We present a groundwork study into tidal waves in neutron star oceans and their consequences. Specifically, we investigate how oscillation modes in neutron star oceans can be tidally excited during compact binary inspirals and parabolic encounters. We find that neutron star oceans can sustain tidal waves with frequencies between 0.01 and 20 Hz. Our results suggest that tidally resonant neutron star ocean waves may serve as a never-before studied source of precursor electromagnetic emission prior to neutron star–black hole and binary neutron star mergers. If accompanied by electromagnetic flares, tidally resonant neutron star ocean waves, whose energy budget can reach 1046erg, may serve as early warning signs (≳1 min before merger) for compact binary mergers. Similarly, excited ocean tidal waves will coincide with neutron star parabolic encounters. Depending on the neutron star ocean model and a flare emission scenario, tidally resonant ocean flares may be detectable byFermiand Nuclear Spectroscopic Telescope Array (NuSTAR) out to ≳100 Mpc with detection rates as high as ∼7 yr−1for binary neutron stars and ∼0.6 yr−1for neutron star–black hole binaries. Observations of emission from neutron star ocean tidal waves along with gravitational waves will provide insight into the equation of state at the neutron star surface, the composition of neutron star oceans and crusts, and neutron star geophysics.