论文标题
全息恒星的正常和准标准模式
Normal and Quasinormal Modes of Holographic Multiquark Star
论文作者
论文摘要
多Quark恒星的四倍正常模式振荡频率$ f_ {n} $以$ n = 1-5 $计算。在核心区域中从低密度多Quark的过渡时，前2个模式跳至较大的值，这是高密度核心存在的独特标志。当恒星振荡与时空振荡夫妇时，将产生重力波（GW），并且恒星将经历震动的振荡。振荡的准模式〜（QNM）是使用两种直接扫描和WKB计算的，分别针对具有大小假想部分的QNM。小型虚构QNM的频率$ 1.5-2.6 $ kHz和缩减时间$ 0.19-1.7 $ secs的多Quark Star，质量$ M = 0.6-2.1 m _ {\ odot} $〜（太阳能质量）。具有大型虚部零件的WKB QNM $ 5.98-9.81 $ kHz和阻尼时间$ 0.13-0.46 $ MS，$ M \ simeq 0.3-2.1 m _ {\ odot} $。他们被认为是流体$ f-$模式和时空曲率$ w-$模式。
The quadrupole normal-mode oscillation frequency $f_{n}$ of multiquark star are computed for $n=1-5$. At the transition from low to high density multiquark in the core region, the first 2 modes jump to larger values, a distinctive signature of the presence of the high-density core. When the star oscillation couples with spacetime, gravitational waves~(GW) will be generated and the star will undergo damped oscillation. The quasinormal modes~(QNMs) of the oscillation are computed using two methods, direct scan and WKB, for QNMs with small and large imaginary parts respectively. The small imaginary QNMs have frequencies $1.5-2.6$ kHz and damping times $0.19-1.7$ secs for multiquark star with mass $M=0.6-2.1 M_{\odot}$~(solar mass). The WKB QNMs with large imaginary parts have frequencies $5.98-9.81$ kHz and damping times $0.13-0.46$ ms for $M\simeq 0.3-2.1 M_{\odot}$. They are found to be the fluid $f-$modes and spacetime curvature $w-$modes respectively.
