论文标题
温度对中子星的核心G模型的影响
Temperature Effects on Core g-modes of Neutron Stars
论文作者
论文摘要
中子星提供了一个独特的物理实验室，以高密度研究物质的特性。我们研究了由浮力驱动的高密度物质组成的诊断。潮汐力可以激发这些振荡，并将夫妇降至引力波。我们使用Raithel，Özel和Psaltis最近提出的有限温度效应的参数化，将冷中子星物质的G模式光谱扩展到预期在中子星合并中获得的温度。我们发现，在高温下抑制了规范质量中子星（$ \ $ \ $ 1.4 $ m _ {\ odot} $）的G模型，并且仅在最大的巨大（$ \ geq $ 2 $ 2 $ M _ {\ odot} $）中支持核心$ g $ -modes。
Neutron stars provide a unique physical laboratory to study the properties of matter at high density. We study a diagnostic of the composition of high-density matter, namely, g-mode oscillations, which are driven by buoyancy forces. These oscillations can be excited by tidal forces and couple to gravitational waves. We extend prior results for the g-mode spectrum of cold neutron star matter to temperatures that are expected to be achieved in neutron star mergers using a parameterization for finite-temperature effects recently proposed by Raithel, Özel and Psaltis. We find that the g-modes of canonical mass neutron stars ($\approx$1.4$M_{\odot}$) are suppressed at high temperature, and core $g$-modes are supported only in the most massive ($\geq $2$M_{\odot}$) of hot neutron stars.
