论文标题
通过重力波和中子星的二进制中的强磁化等离子体之间的耦合激发的磁性水力学波激发
Magnetohydrodynamic waves excited by a coupling between gravitational waves and a strongly magnetized plasma in binaries of neutron stars
论文作者
论文摘要
二进制中子星（BNSS）的合并是能够通过地面干涉探测器检测到的引力波（GWS）的来源之一。该事件GW170817是在引力和电磁光谱中首次观察到的事件，通过该联合分析显示了与短伽马射线爆发（SGRB）模型的一定兼容性，以解释该系统的签名。由于中子星的强烈磁场，等离子体磁层保持了强烈的磁化，而GW通过等离子体的传播可以激发磁流失动力学（MHD）模式，例如AlfVén和磁性波。 MHD模式通过等离子体携带能量和动量，提出了一种在二进制过程中加速物质的机制，解释了SGRB的火球模型的某些特征。我们提出了一种半分析形式主义，以确定恒星灵感阶段中GW-MHD相互作用传递的能量。使用GW170817的推断物理参数，我们表明血浆中的能量可以达到最大值$ \ sim 10^{35} \，{\ rm j} $（$ \ sim 10^{32}} {32}} \，{\ rm j} $）对于AlfVUn Mode（If Alfvun Magnetoson Mode）（IF MAGNETOSONIC）INGW $θ=π/ 4 $。特别是，对于$θ=π/ 2 $，仅磁性模式与GWS保持一致。在这种情况下，等离子体中的激发能量达到最大值$ \ sim 10^{36} {\ rm j} $。如果事件GW170817的祖细胞表面上的磁场为$ \ sim 2 \ times 10^{9} \，{\ rm t} $，则可以获得与GRB 170817A推断的能量相当的能量。特别是，我们的半分析形式主义与其他作者通过完整的一般相对论磁性水力学（GRMHD）模拟获得的结果一致。 [简略]
Coalescence of binary neutron stars (BNSs) is one of the sources of gravitational waves (GWs) able to be detected by ground-based interferometric detectors. The event GW170817 was the first observed in the gravitational and electromagnetic spectra, showing through this joint analysis a certain compatibility with the models of short gamma-ray bursts (sGRBs) to explain the signature of this system. Due to the intense magnetic fields of the neutron stars, the plasma magnetosphere stays strongly magnetized and the propagation of the GW through plasma can excite magnetohydrodynamic (MHD) modes such as Alfvén and magnetosonic waves. The MHD modes carry energy and momentum through the plasma, suggesting a mechanism to accelerate the matter during the coalescence of the binaries, explaining some characteristics of the fireball model of the sGRBs. We present a semianalytical formalism to determine the energy transferred by the GW-MHD interaction during the inspiral phase of the stars. Using the inferred physical parameters for GW170817, we show that the energy in the plasma can reach maximum value $\sim 10^{35}\,{\rm J}$ ($\sim 10^{32}\,{\rm J}$) for the Alfvén mode (magnetosonic mode) if the angle formed between the background magnetic field and the GW propagation direction is $θ= π/ 4$. Particularly, for $θ= π/ 2$ only the magnetosonic mode is in coherence with the GWs. In this case, the excited energy in the plasma reaches maximum value $\sim 10^{36} {\rm J}$. If the magnetic field on the surface of the progenitors of the event GW170817 was $\sim 2\times 10^{9}\,{\rm T}$ then energies comparable to those inferred for the GRB 170817A could be obtained. In particular, our semianalytical formalism show consistence with the results obtained by other authors through full general relativistic magnetohydrodynamics (GRMHD) simulations. [ABRIDGED]
