More than two dozen soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) have been detected so far. These are isolated compact objects. Many of them are either found to be associated with supernova remnants or their surface magnetic fields are directly measured, confirming that they are neutron stars (NSs). However, it has been argued that some SGRs and AXPs are highly magnetized white dwarfs (WDs). Meanwhile, the existence of super-Chandrasekhar WDs has remained to be a puzzle. However, not even a single such massive WD has been observed directly. Moreover, some WD pulsars are detected in electromagnetic surveys and some of their masses are still not confirmed. Here we calculate the signal-to-noise ratio for all these objects, considering different magnetic field configurations and thereby estimate the required time for their detection by various gravitational wave (GW) detectors. For SGRs and AXPs, we show that, if these are NSs, they can hardly be detected by any of the GW detectors, while if they are WDs, Big Bang Observer (BBO), DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) and Advanced Laser Interferometer Antenna (ALIA) would be able to detect them within a few days to a year of integration, depending on the magnetic field strength and its configuration. Similarly, if a super-Chandrasekhar WD has a dominant toroidal field, we show that even Laser Interferometer Space Antenna (LISA) and TianQin would be able to detect it within one year of integration. We also discuss how GWs can confirm the masses of the WD pulsars.
Prospects of calibrating afterglow modeling of short GRBs with gravitational wave inclination angle measurements and resolving the Hubble tension with a GW-GRB association event
Thick Lunar Crust Amplifies Deci-Hertz Gravitational-Wave Signal
Institute of Geology and Geophysics, Chinese Academy of Sciences（中国科学院地质与地球物理研究所）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）
A thorough investigation of cross-correlation estimators for stochastic gravitational-wave background searches in ground-based detector data
University of Minnesota（明尼苏达大学）；University of Texas Rio Grande Valley（德克萨斯大学里奥格兰德河谷分校）；Inter-University Centre for Astronomy and Astrophysics（大学间天体物理中心）；ETH Zurich（苏黎世联邦理工学院）
Prospects of resolving and localising individual supermassive black hole binaries with pulsar timing arrays: the host ranking challenge
Washington State University（华盛顿州立大学）；Institute of Astrophysics, FORTH（FORTH天体物理研究所）；Vanderbilt University（范德堡大学）；Fisk University（菲斯克大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）
Efficient Evaluation of Gravitational Lensing Amplification Factors: A Deep Learning Framework
Zhejiang University（浙江大学）；Massachusetts Institute of Technology（麻省理工学院）；Wuhan University（武汉大学）；Institute of Mechanics, Chinese Academy of Sciences（中国科学院力学研究所）
