Progress of the investigation for thermal effect in space GW detection mission TianQin @LISAcommunity

Uploaded July 2022 | Updated September 2026, 2 hours ago

TianQin is a proposal for a space-borne detector of gravitational waves in the millihertz frequencies. The inertial sensor is one of the most important payloads. Its resolution is related to the non-gravitation disturbance on the test mass. The test mass will be disturbed by a thermal gradient on both sides of the sensitive axis, and we term this disturbance thermal effect. It includes radiometer effect, radiation pressure effect, and asymmetric outgassing. The specific action mechanism of asymmetric outgassing is still not clear. It can only be measured by experiments. Therefore, we aim to reveal the mechanism of asymmetric outgassing and evaluate the contribution of the thermal effect in the TianQin project.

We developed a TianQin inertial sensor simulation device with a resolution of 15 fNm/âˆšHz @0.4 mHz . Some NTC heaters and thermometers are installed outside the X-axis plate to produce a temperature difference of the order of 10 mk with a period of 2400 s. Then the contribution of the thermal effect produced by periodic temperature modulation is measured by an autocollimator. Finally, the contribution of the outgassing effect is obtained by data processing.

The device can currently measure the thermal effect under a variety of thermal gradients, ambient temperatures, and pressures. It can also measure and evaluate the outgassing effect. We will further study and control the outgassing effect by changing the plate with difierent material and baking under different conditions. The achievements of this study can provide some instructions for the development of the inertial sensor for gravitational wave detection missions.

Authors: Guilin Li, Li Liu, Zebing Zhou
Presenter: Guilin Li

Progress of the investigation for thermal effect in space GW detection mission TianQin

$AMIGO: Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Astrodynamical middle-frequency interferometric gravitational wave observatory Wei-Tou Ni, Gang Wang and An-Ming Wu AMIGO is a first-generation Astrodynamical Middle-frequency Interferometric GW Observatory. The scientific goals of AMIGO are: to bridge the spectra gap between first-generation high-frequency and low-frequency GW sensitivities; to detect intermediate mass BH coalescence; to detect inspiral phase and predict time of binary black hole coalescence together with neutron star coalescence for ground interferometers; to detect compact binary inspirals for studying stellar evolution and galactic population. The mission concept is to use time delay interferometry for a nearly triangular formation of 3 drag-free spacecraft with nominal arm length 10,000 km, emitting laser power 2-10 W and telescope diameter 300-500 mm. The design GW sensitivity in the middle frequency band is 3 x 10^(-21) Hz^(-1/2). Both heliocentric and geocentric orbits are under study. All options have LISA-like formations, that is the triangular formation is 60 deg inclined to the orbit plane. For AMIGO, the first-generation time delay interferometry is good enough for the laser frequency noise suppression. We also investigate for each options of orbits under study, whether constant equal-arm implementation is feasible. For the solar-orbit option, the acceleration to maintain the formation can be designed to be less than 15 nm/s2 with the thruster requirement in the 15 {mu}N range. AMIGO would be a good place to implement the constant equal-arm option. Fuel requirement, thruster noise requirement and test mass acceleration actuation requirement are briefly considered. From the orbit study, the solar orbit option is the first mission orbit choice. We study the deployment for this orbit option. A last-stage launch from 300 km LEO (Low Earth Orbit) to an appropriate 2-degree-behind-the-Earth AMIGO formation in 95 days requires only a {delta}v of 75 m/s.$

Resolving Galactic binaries using a network of space-borne gravitational wave detectors

Highlighting a milestone for LISA: Our understanding and long-term results of LPF interferometry

LISA Symposium XIV Parallel B Cosmology part 1

Applying machine learning methods to MBHB parameter estimation

Rapid detectability estimation for extreme mass ratio inspiral populations using machine learning