Conveners
Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methods: Tuesday block 1
- Wei-Tou Ni (Innovation Academy of Precision Measuremnt Sciencs and Technology of Chinese Academy of Sciences)
- Gang Wang (Shanghai Astronomical Observatory, CAS)
Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methods: Tuesday block 2
- Wei-Tou Ni (Innovation Academy of Precision Measuremnt Sciencs and Technology of Chinese Academy of Sciences)
- Gang Wang (Shanghai Astronomical Observatory, CAS)
Description
The micro-Hz GW (Gravitational Wave) band, ranging from 0.1 to 100 μHz, occupies a crucial intermediate gap between the PTA (Pulsar Timing Array) GW detection band (0.03—100 nHz) and the sensitive bands of space missions like LISA/Taiji/TianQin (0.1 mHz—1 Hz). This frequency range is abundant with potential GW sources. The primary scientific objectives within this band include the detection of GWs from supermassive BH (Black Hole) binary inspiral and coalescence events spanning masses of 10^5-10^10 solar masses, as well as GWs emitted during the inspiral phase of intermediate-mass BH coalescence and intermediate BH binaries falling into supermassive BHs. Detection micro-Hz GWs will provide opportunities to study the BH co-evolution with the galaxies, to test general relativity and beyond-the Standard-Model theories, to explore the micro-Hz stochastic GW background and so on. Several detection proposals under study, including ASTROD-GW, Folkner’s mission, LISAmax, Super-ASTROD, μAries, optical clock missions, and AI (Atomic Interferometry) missions. We solicit new ideas and progress papers together with multi-band and multi-messenger papers for this parallel session.
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Wei-Tou Ni (State Key Laboratory of Magnetic Resonance and Atomic and Molecular Physics, Innovation Academy for Precision Measurement Science and Technology, Chinese Academy of Sciences, Wuhan 430071, China)09/07/2024, 15:00Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsTalk in a parallel session
Micro-Hertz Gravitational Waves (0.1-100 Hz): Overview of Sources and Detection Methods
Wei-Tou Ni and Gang Wang
The micro-Hz GW (Gravitational Wave) band, ranging from 0.1 to 100 Hz, occupies a crucial intermediate gap between the PTA (Pulsar Timing Array) GW detection band (0.03—100 nHz) and the sensitive bands of space missions like LISA/Taiji/TianQin (0.1 mHz—1 Hz). This frequency...
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Peng Xu (Institute of Mechanics, Chinese Academy of Sciences)09/07/2024, 15:25Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsInvited talk in a parallel session
Coalescing supermassive black hole binaries (SMBHBs) are the primary source candidates for low frequency gravitational wave (GW) detections, which could bring us deep insights into galaxy evolutions over cosmic time and violent processes of spacetime dynamics. Promising candidates had been found based on optical and X-ray observations, which claims for new and ready-to-use GW detection...
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Jun Zhang (International Center for Theoretical Physics Asia-Pacific)09/07/2024, 16:05Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsTalk in a parallel session
Gravitational waves provide a unique probe to physics in strong gravity regime and dark sector of our universe. In this talk, we will discuss the effects of ultralight fields on binary inspirals, assuming the fields are significantly excited by neutron stars or black holes in the binaries. We will report on a search for axion-like particles by analyzing the gravitational waves from the binary...
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Soumen Mondal (Jadavpur University, Kolkata, India)09/07/2024, 17:00Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsTalk in a parallel session
Real extreme/intermediate-mass ratio inspiral (E/IMRI) systems are likely to contain large accretion discs which could be as massive as the central supermassive black hole. Therefore, contrary to its ideal model, a real E/IMRI system contains a third important component: the accretion disc. We study the influence of these discs on the emitted gravitational wave (GW) profile and its...
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Wei-Tou Ni (Innovation Academy of Precision Measuremnt Sciencs and Technology of Chinese Academy of Sciences), Prof. Wei-Tou Ni (State Key Laboratory of Magnetic Resonance and Atomic and Molecular Physics, Innovation Academy for Precision Measurement Science and Technology, Chinese Academy of Sciences, Wuhan 430071, China)09/07/2024, 17:20Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsTalk in a parallel session
ASTROD-GW is designed to observe gravitational waves in the micro-Hz frequency band, employing three spacecraft near the Sun–Earth Lagrange points L3, L4, and L5 to form triangular interferometers with a 2.6 AU arm length. Benefiting from the relative gravitational stabilities of the Lagrange points in 30 years, the mission orbit can remain stable for more than 10 years. The antenna pattern of...
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Gang Wang (Shanghai Astronomical Observatory, CAS)09/07/2024, 17:40Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsInvited talk in a parallel session
A large number of galactic binary systems emit gravitational waves (GW) continuously with frequencies below ∼10 mHz. The LISA mission could identify tens of thousands of binaries over years of observation and will be subject to the confusion noise around 1 mHz yielded by the unresolved sources. Beyond LISA, there are several missions have been proposed to observe GWs in the sub-mHz range where...
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Renjie Wang (HIAS, UCAS)09/07/2024, 18:00Micro-Hertz gravitational waves (0.1-100 μHz): sources and detection methodsInvited talk in a parallel session
The future space-borne gravitational wave(GW) missions will be able to detect abundant gravitational wave signals in the micro-Hz band. The gravitational wave mission, ASTROD-GW can bridge the gap between the millihertz and nanohertz bands and has a great potential to detect the supermassive black hole binary coalescence events. A large number of galactic binaries will continuously emit GW...
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