Conveners
Mid-frequency gravitational waves (0.1-10 Hz): sources and detection methods: Thursday block 1
- Wei-Tou Ni (Innovation Academy of Precision Measuremnt Sciencs and Technology of Chinese Academy of Sciences)
- Youjun Lu (National Astronomical Observatories of China)
Mid-frequency gravitational waves (0.1-10 Hz): sources and detection methods: Thursday block 2
- Wei-Tou Ni (Innovation Academy of Precision Measuremnt Sciencs and Technology of Chinese Academy of Sciences)
- Youjun Lu (National Astronomical Observatories of China)
Description
The mid-frequency GW (Gravitational Wave) band (0.1-10 Hz) between the LIGO-Virgo-KAGRA detection band and LISA-TAIJI/TIANQIN detection band is rich in GW sources. In addition to the intermediate BH (Black Hole) Binary coalescence, GWs can also come from the inspiral phase of stellar-mass coalescence and from compact binaries falling into intermediate BHs. Detecting mid-frequency GWs enables us to study the compact object population, to test general relativity and beyond-the Standard-Model theories, to explore the stochastic GW background and so on. In addition to DECIGO and BBO, the detection proposals under study include AEDGE, AIGSO, AION, AMIGO, B-DECIGO, DO, ELGAR, GLOC, INO, LGWA, MAGIS, MIGA, SOGRO, TIAGO, TOBA, ZAIGA, etc. Great advances have accumulated since MG16. We solicit progress papers and new ideas for this parallel session.
Mid-frequency Gravitational Waves (0.1-10 Hz): Overview of Sources and Detection Methods
Youjun Lu and Wei-Tou Ni
The mid-frequency GW (Gravitational Wave) band (0.1-10 Hz) between the LIGO-Virgo-KAGRA detection band and LISA-TAIJI/TIANQIN detection band is rich in GW sources. In addition to the intermediate BH (Black Hole) Binary coalescence, GWs can also come from the inspiral phase...
The ground-based gravitational wave (GW) observations discover a population of merging stellar binary black holes (BBHs), which could also be detected by the space-based low-frequency GW detectors, such as LISA, Taiji and Tianqin, in their early inspiral stages. The middle-frequency GW band, a missing link between the high-frequency and low-frequency band, is an important piece for multiband...
ZAIGA (the Zhaoshan long-baseline Atom Interferometer Gravitation Antenna) is a proposed underground long-baseline atom interferometer (AI) facility, aiming for experimental research on gravitation and related problems. It includes gravitational wave detection (ZAIGA-GW), dark matter detection (ZAIGA-DM), high-precision test of the equivalence principle of micro-particles (ZAIGA-EP),...
For space gravitational wave (GW) detection, arm locking is a proposal useful in decreasing the frequency noise of the laser sources for current developing space missions LISA and Taiji/TianQin. In this talk, we discuss the application of arm locking to the Astrodynamical Middle-frequency Interferometric Gravitational Observatory (AMIGO) to decrease the frequency noise of laser sources. For...
Gravitational-wave astronomy has achieved remarkable progress over the
past decades, detecting waves across a wide range of frequencies.
However, the band around one Hz remains unexplored. This band is vital
for studying some of the most fascinating sources, including
intermediate-mass binary black hole mergers, early inspiralling compact
binaries, and possibly cosmic inflation. The...
In the space gravitational wave detection program, the locking and releasing of test mass is one of the key technologies. The test mass is locked in during the launch phase of the spacecraft and then released during the scientific exploration phase, allowing it to go into free fall. Among them, the residual release impulse of the test mass is required to be in the order of magnitude of 10-5 kg...
