Test of the Weak Equivalence Principle using LIGO observations of GW150914 and Fermi observations of GBM transient 150914
Test of the Weak Equivalence Principle using LIGO observations of GW150914 and Fermi observations of GBM transient 150914
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使用 GW150914 的 LIGO 观测值和 GBM 瞬态 150914 的费米观测值测试弱等效原理
DOI：
10.1016/j.physletb.2017.04.033
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发表时间：
2017
影响因子：
4.4
通讯作者：
Xu Lixin
中科院分区：
文献类型：
--
作者：
Liu Molin;Zhao Zonghua;You Xiaohe;Lu Jianbo;Xu Lixin
大约0.4 S在激光干涉仪引力波天文台探测到一个瞬变引力波信号GW150914之后，费米伽马射线爆发监测器也发现了一个微弱的电磁瞬变(GW瞬变150914)。时间和位置重合有利于GW150904和GBM瞬变150914之间的可能关联。在这种可能的关联下，我们采用费米电磁(EM)局域化，并从两个事件的观测中推导出对可能违反弱等价原理(WEP)的约束。我们的计算基于四个比较：(1)第一个是在两个LIGO站点探测到的初始GW的比较。从这些初始GW的不同极化，我们得到了参数化后牛顿参数Δγ≲10−10的任何差异的极限。(2)第二个是GW和可能的电磁波的比较。利用传统的超爱丁顿吸积模型，我们再次得到了量子数为150914的超爱丁顿吸积模型的上限为Δγ≲10−10。与前人关于光子和中微子的结果相比，我们的极限比耀斑中的PeV中微子强5个数量级，比SN1987A的MeV中微子强7个数量级。(3)第三个是在[35 Hz，250 Hz]范围内不同频率的GW的比较。最后两次比较得出了一个更强的极限，Δγ≲10−8。我们的结果突出了多信使信号利用不同发射通道来加强现有WEP测试的潜力。
About 0.4 s after the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a transient gravitational-wave (GW) signal GW150914, the Fermi Gamma-ray Burst Monitor (GBM) also found a weak electromagnetic transient (GBM transient 150914). Time and location coincidences favor a possible association between GW150904 and GBM transient 150914. Under this possible association, we adopt Fermi's electromagnetic (EM) localization and derive constraints on possible violations of the Weak Equivalence Principle (WEP) from the observations of two events. Our calculations are based on four comparisons:(1) The first is the comparison of the initial GWs detected at the two LIGO sites. From the different polarizations of these initial GWs, we obtain a limit on any difference in the parametrized post-Newtonian (PPN) parameter Δ γ≲ 10− 10.(2) The second is a comparison of GWs and possible EM waves. Using a traditional super-Eddington accretion model for GBM transient 150914, we again obtain an upper limit Δ γ≲ 10− 10. Compared with previous results for photons and neutrinos, our limits are five orders of magnitude stronger than those from PeV neutrinos in blazar flares, and seven orders stronger than those from MeV neutrinos in SN1987A.(3) The third is a comparison of GWs with different frequencies in the range [35 Hz, 250 Hz].(4) The fourth is a comparison of EM waves with different energies in the range [1 keV, 10 MeV]. These last two comparisons lead to an even stronger limit, Δ γ≲ 10− 8. Our results highlight the potential of multi-messenger signals exploiting different emission channels to strengthen existing tests of the WEP.