Eddington激发的Born-Infeld引力中的恒星振荡
Stellar oscillations in Eddington-inspired Born-Infeld gravity
摘要：
我们考虑了相对论性恒星在Eddington启发的Born-Infeld引力（EiBI）中的恒星振荡。为了研究特定的频率，我们通过线性化场方程推导出EiBI中控制恒星振荡的微扰方程，并通过数值计算确定EiBI，$κ$和恒星模型中耦合参数变化时的振荡频率。结果发现，频率与$κ$的值有很强的依赖关系，其中具有负的$κ$的EiBI中的频率变得更高，而具有正的$κ$的EiBI中的频率变得更低，这比广义相对论中的期望值要低。我们还发现，通过对基频的观测，可以将EiBI与$8πε_0|κ|\gtrsim 0.03$从广义相对论中区分出来，而与中子星物质的状态方程无关，其中$ε_0$表示核饱和密度，$ε_0κ$成为无量纲参数。随着对EOS的进一步限制，人们甚至可以将EiBI与$8πε_0|κ|\lesssim 0.03$和广义相对论区分开来。
英文摘要：
We consider the stellar oscillations of relativistic stars in the Eddington-inspired Born-Infeld gravity (EiBI). In order to examine the specific frequencies, we derive the perturbation equations governing the stellar oscillations in EiBI by linearizing the field equations, and numerically determine the oscillation frequencies as changing the coupling parameter in EiBI, $κ$, and stellar models. As a result, we find that the frequencies depend strongly on the value of $κ$, where the frequencies in EiBI with negative $κ$ become higher and those with positive $κ$ become lower than the expectations in general relativity. We also find that, via the observation of the fundamental frequency, one could distinguish EiBI with $8πε_0|κ|\gtrsim 0.03$ from general relativity, independently of the equation of state (EOS) for neutron star matter, where $ε_0$ denotes the nuclear saturation density and $ε_0κ$ become dimensionless parameter. With the further constraints on EOS, one might distinguish EiBI even with $8πε_0|κ|\lesssim 0.03$ from general relativity.
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