A coupling system between Gaussian type-microwave photon flux, static magnetic field and fractal membranes (or other equivalent microwave lenses) can be used to detect high-frequency gravitational waves (HFGWs) in the microwave band. We study the signal photon flux, background photon flux and the requisite minimal accumulation time of the signal in the coupling system. Unlike pure inverse Gertsenshtein effect (G-effect) caused by the HFGWs in the GHz band, the the electromagnetic (EM) detecting scheme (EDS) proposed by China and the US HFGW groups is based on the composite effect of the synchro-resonance effect and the inverse G-effect. Key parameters in the scheme include first-order perturbative photon flux (PPF) and not the second-order PPF; the distinguishable signal is the transverse first-order PPF and not the longitudinal PPF; the photon flux focused by the fractal membranes or other equivalent microwave lenses is not only the transverse first-order PPF but the total transverse photon flux, and these photon fluxes have different signal-to-noise ratios at the different receiving surfaces. Theoretical analysis and numerical estimation show that the requisite minimal accumulation time of the signal at the special receiving surfaces and in the background noise fluctuation would be $\sim10^3-10^5$ seconds for the typical laboratory condition and parameters of $h_{r.m.s.}\sim10^{-26}-10^{-30}$ at 5GHz with bandwidth $\sim$1Hz. In addition, we review the inverse G-effect in the EM detection of the HFGWs, and it is shown that the EM detecting scheme based only on the pure inverse G-effect in the laboratory condition would not be useful to detect HFGWs in the microwave band.
Bounded Electromagnetic Power Flux at Naked Kasner Singularities
Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET)（阿根廷国家科学研究委员会）；Instituto Balseiro (UNCUYO)（巴尔塞罗研究所）；Universidad Diego Portales（迭戈·波特莱斯大学）；Universidad de La Serena（拉塞雷纳大学）
这是M.B.Mensky论文的英文翻译，见：K. P. Stanyukovich（编辑），“引力理论和基本粒子问题“，第6期，莫斯科，原子化，1975年，第181 -190页（俄文）。本文进一步阐述了Braginsky和Mensky于1971年提出的通过观察引力波对封闭谐振腔（波导）中电磁波的谐振作用来探测高频引力波的思想。这种探测器背后的现象被称为引力电磁共振（GER）。在本文中，封闭的（例如圆形）谐振腔或波导和长波导（例如螺旋形）被认为是可能的引力波探测器。高频引力波探测器现在再次成为现实（见A.M.Cruise和R. M. J. Ingley，Class。定量重力22，S479，2005），但目前关于这一主题的文献并没有涵盖本文讨论的所有问题。
Electromagnetic alignment and jet precession around supermassive black holes: Quasi-periodic oscillations in tidal disruption events
Universitat Politècnica de València（瓦伦西亚理工大学）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；The Kavli Institute for Astronomy and Astrophysics（卡弗里天文学与天体物理研究所）；Beijing Institute of Mathematical Sciences and Applications（北京数学与应用科学研究所有限公司）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）
Detecting electromagnetic counterparts to LIGO/Virgo/KAGRA gravitational wave events with DECam: Neutron Star Mergers
Carnegie Mellon University（卡内基梅隆大学）；University of Chicago（芝加哥大学）；University of Ferrara（费拉拉大学）；INFN, Sezione di Ferrara（意大利国家核物理研究所费拉拉分部）；INAF, Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Universität Potsdam（波茨坦大学）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；Utrecht University（乌得勒支大学）；Nikhef（荷兰国家核物理与粒子物理研究所）；California Institute of Technology（加州理工学院）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）
On the possibility of detecting ultra-short period exoplanets with LISA
Cunha等人（2018）最近重新研究了从系外行星探测引力波的可能性，声称LISA将观测到三个超短周期系统。我们重新审视他们的分析，并得出结论，目前已知的系外行星系统是不太可能被检测到的，即使假设一个LISA观测时间$T_{\rm obs}=4$ yrs.Conclusive声明对这些系统之一，GP Com B的可检测性，将需要更好地了解系统的属性，以及更仔细的建模LISA的响应和银河系的混乱噪音。尽管如此，用LISA探测系外行星的可能性仍然很有趣，值得进一步研究，因为引力波可能产生难以用电磁观测约束的动力学性质。
