r模的黏性阻尼与引力波辐射
Viscous damping of r-modes and emission of gravitational waves
AI总结：
本研究针对脉冲星r模这一稳定引力波源，分析刚性壳层的黏性阻尼效应，采用指定物态方程与慢转近似估算引力波强度，并计算了不同质量脉冲星的临界频率等自旋相关参数。
摘要：
本研究探索了脉冲星中的罗斯比模（r模）扰动作为稳定引力波（GW）源的相关特性，分析了刚性壳层对流体核与壳层间边界层内黏性阻尼及耗散率的影响。研究采用慢转近似，结合由APR与Skyrme有效相互作用（采用Brussels-Montreal参数组）推导的物态方程，估算了以应变张量振幅表征的引力波辐射强度。研究设定中子星核为包含中子、质子、电子和μ子的β平衡核物质，外围包裹固态壳层，并针对大质量范围内的脉冲星计算了临界频率、自旋频率的时间演化及变化率。
英文摘要：
The Rossby mode (r-mode) perturbation in pulsars as a steady gravitational wave (GW) source has been explored. The effect of a rigid crust on viscous damping and dissipation rate in the boundary layer between fluid core and crust has been studied. The intensity of the emitted GWs in terms of the strain tensor amplitude has been estimated with the approximation of slow rotation using equation of state derived from the APR and Skyrme effective interactions with Brussels-Montreal parameter sets. The core of the neutron star has been considered to be $β$-equilibrated nuclear matter containing neutrons, protons, electrons and muons, surrounded by a solid crust. Calculations have been made for critical frequencies, the time evolution and the rate of change of the spin frequencies across a broad spectrum of pulsar masses.
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