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arXiv 2005.04127hep-phgr-qchep-th
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Kaluza-Klein重共振的引力印记

Gravitational Imprints from Heavy Kaluza-Klein Resonances

Eugenio Megias, Germano Nardini, Mariano Quiros

备注：
11 pages, 6 figures; v2 extended version: added references and Figs. 1 (right), 2, 3, 4 (lower panels) and 5, Sec. IV, and extended discussion in Secs. V, VI and VII; v3 added references, extended discussion in Sec. VI. It matches the version published in Physical Review D
发表信息：
Phys. Rev. D 102, 055004 (2020)
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摘要：

本文系统地研究了具有类幂行为标量势的五维弯曲模型中辐射场的全息相变。我们认为卡鲁扎-克莱因（KK）共振质量$m_{\rm KK}$在TeV尺度或以上。利用超势形式考虑了辐射场对引力度规的反作用。禁闭/解除禁闭一级相变导致引力波随机背景，该背景主要依赖于对偶理论中的尺度$m_{\rm KK}$和颜色数$N$.其功率谱的峰值频率取决于电弱扇区所需的调谐量。事实证明，现在和即将到来的引力波观测站可以探测KK共振非常重的情况。目前的aLIGO数据已经排除了质量在$m_{\rm KK}\sim(1 - 10) \times 10^5$ TeV区间的矢量玻色子KK共振。未来的引力实验将对质量为$m_{\rm KK}\lesssim 10^5$ TeV（LISA）、$10^8$ TeV（aLIGO Design）和$10^9$ TeV（ET）的共振敏感。最后，我们还发现，在频谱上的大爆炸核合成的约束变成了一个较低的约束的成核温度为$T_n \gtrsim 10^{-4}\sqrt{N} \,m_{\rm KK}$。

英文摘要：

We systematically study the holographic phase transition of the radion field in a five-dimensional warped model which includes a scalar potential with a power-like behavior. We consider Kaluza-Klein (KK) resonances with masses $m_{\rm KK}$ at the TeV scale or beyond. The backreaction of the radion field on the gravitational metric is taken into account by using the superpotential formalism. The confinement/deconfinement first order phase transition leads to a gravitational wave stochastic background which mainly depends on the scale $m_{\rm KK}$ and the number of colors, $N$, in the dual theory. Its power spectrum peaks at a frequency that depends on the amount of tuning required in the electroweak sector. It turns out that the present and forthcoming gravitational wave observatories can probe scenarios where the KK resonances are very heavy. Current aLIGO data already rule out vector boson KK resonances with masses in the interval $m_{\rm KK}\sim(1 - 10) \times 10^5$ TeV. Future gravitational experiments will be sensitive to resonances with masses $m_{\rm KK}\lesssim 10^5$ TeV (LISA), $10^8$ TeV (aLIGO Design) and $10^9$ TeV (ET). Finally, we also find that the Big Bang Nucleosynthesis bound in the frequency spectrum turns into a lower bound for the nucleation temperature as $T_n \gtrsim 10^{-4}\sqrt{N} \,m_{\rm KK}$.

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