混合星中的不连续重力模：评估快速和慢速相位转换的作用
Discontinuity gravity modes in hybrid stars: assessing the role of rapid and slow phase conversions
摘要：
当恒星内部存在急剧的密度跳跃时，扰动夸克-强子混合星可能会出现不连续引力模，这是推断致密天体中夸克物质核心存在的潜在指纹。当混合星受到扰动时，夸克-强子界面可能发生转换反应，并可能对恒星的动力学稳定性和准简正模谱等全局性质起关键作用。在这项工作中，我们研究的转化率在界面上的作用。为此，我们首先推导出在缓慢和快速转换的情况下，在非径向扰动混合星的尖锐界面处的结条件。然后，我们分析了在这两种情况下的不连续$g$模式。对于快速转换，不连续性$g$ -模式具有零频率，因为在相分离表面附近的移位的流体元件几乎立即将其组成调整到其周围，并且重力不能提供浮力。对于慢转换，一个$g$ -模式存在，它的性质进行了分析，在这里使用现代强子和夸克状态方程。此外，最近已经表明，在缓慢转换的情况下，出现稳定的混合构型的扩展分支，其中$\partial M/ \partial ε_c <0$。我们发现，$g$ -模式的标准分支（即，一个与$\partial M/ \partial ε_c > 0$）的频率和阻尼时间与以前的结果在文献中。然而，扩展分支的$g$ -模式具有显著更大的频率（在$1-2 \, \mathrm{kHz}$范围内）和短得多的阻尼时间（在某些情况下为几秒）。我们讨论了探测能力的$g$模式GW与目前和计划GW观测。
英文摘要：
Discontinuity gravity modes may arise in perturbed quark-hadron hybrid stars when a sharp density jump exists in the stellar interior and are a potential fingerprint to infer the existence of quark matter cores in compact objects. When a hybrid star is perturbed, conversion reactions may occur at the quark-hadron interface and may have a key role in global stellar properties such as the dynamic stability and the quasi-normal mode spectrum. In this work we study the role of the conversion rate at the interface. To this end, we first derive the junction conditions that hold at the sharp interface of a non-radially perturbed hybrid star in the case of slow and rapid conversions. Then, we analyse the discontinuity $g$-mode in both cases. For rapid conversions, the discontinuity $g$-mode has zero frequency because a displaced fluid element near the phase splitting surface adjusts almost immediately its composition to its surroundings and gravity cannot provide a buoyancy force. For slow conversions, a $g$-mode exists and its properties are analysed here using modern hadronic and quark equations of state. Moreover, it has been shown recently that in the case of slow conversions an extended branch of stable hybrid configurations arises for which $\partial M/ \partial ε_c <0$. We show that $g$-modes of the standard branch (that is, the one with $\partial M/ \partial ε_c > 0$) have frequencies and damping times in agreement with previous results in the literature. However, $g$-modes of the extended branch have significantly larger frequencies (in the range $1-2 \, \mathrm{kHz}$) and much shorter damping times (few seconds in some cases). We discuss the detectability of $g$-mode GWs with present and planned GW observatories.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
