Orbit design and thruster requirement for various constant arm space mission concepts for gravitational-wave observation

Wang, Gang; Ni, Wei-Tou; Wu, An-Ming

doi:10.1142/s0218271819400066

Cited by 13 publications

(6 citation statements)

References 52 publications

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“…It could also rescale to the recently proposed TianGO GW mission [47] whether it adopted constant arm or not. In accompanying papers, we also study the orbit formations for AIGSO [48,49] and the constant equal-arm orbit options for LISA and TAIJI [50].…”

Section: Discussion and Outlookmentioning

confidence: 99%

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Wang

2020

Int. J. Mod. Phys. D

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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 300-360 mm. The design GW sensitivity in the middle frequency band is 3 × 10 −21 Hz -1 . Four options of orbits are under study: (i) Earth-like solar orbits (2-20 degrees behind the Earth); (ii) 600,000 km high orbit formation around the Earth; (iii) 50,000 km-250,000 high orbit formation around the Earth; (iv) near Earth-Moon L4 (or L5) halo orbit formation. All four options have LISAlike formations, that is the triangular formation is 60º 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/s 2 with the thruster requirement in the 15 μN 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-behindthe-Earth AMIGO formation in 95 days requires only a v of 75 m/s.

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Section: Discussion and Outlookmentioning

confidence: 99%

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Wang

2020

Int. J. Mod. Phys. D

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“…In previous works [73][74][75][76][77][78][79][80], we developed a workflow to design and optimize the orbits for GW space missions by using an ephemeris framework in the solar system barycentric (SSB) coordinates, as well as to calculate the path mismatches between the TDI laser beams. Based on the orbital requirements for new LISA [40], we achieved the numerical orbit for 6 years satisfying the criteria: 1) the relative velocities between S/C are smaller than 5m/s; 2) the changes of breathing angles are less than 1 deg, and 3) the trailing angle is in a range [19°, 23°] [79].…”

Section: Numerical Mission Orbitsmentioning

confidence: 99%

Revisiting time delay interferometry for unequal-arm LISA and TAIJI

Wang

2023

Phys. Scr.

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Three spacecraft of LISA/TAIJI mission follow their respective geodesic trajectories, and their interferometric arms are unequal and time-varying due to orbital dynamics. Time-delay interferometry (TDI) is proposed to suppress the laser frequency noise caused by the unequal-arm. By employing the numerical orbit, we investigate the sensitivity of the first-generation TDI configurations and their corresponding optimal A, E, and T channels. The sensitivities of T channels from Michelson and Monitor/Beacon configurations diverge from the equal-arm case in frequencies lower than 10 mHz, and their performances vary with the inequality of the arm lengths. The mismatches of the laser beam paths are evaluated in a dynamic case, and the residual laser noise in the first-generation TDI could not satisfy the mission requirement.

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“…The relative time t rel would differ from starting t rel = 0 due to the relative motion between the S/C during TDI which is the path mismatch δt. In previous works [38][39][40][41][42][43][44][45], we implemented this algorithm to calculate the path mismatch for laser frequency noise suppression and verify the feasibility of the TDI configurations. Another purpose of the calculation is to determine time delay in each link and the S/C positions, since the response to a GW signal will depend on the time delay factors and instantaneous positions of the S/C, and the noises in the TDI channels are related to the time delay.…”

Section: Numerical Algorithm For Tdi Calculation a Algorithm For Tdi ...mentioning

confidence: 99%

“…We developed a numerical algorithm to calculate the path mismatches in the TDI for LISA-like missions and ASTROD-GW concept since 2011 [37][38][39][40][41][42][43][44][45]. In previous paper [46], by using a set of numerical orbit, we investigated the GW response, noise level and averaged sensitivity of the optimal channels (A, E, and T) constructed from the first-generation Michelson TDI channels (X, Y, and Z) for LISA and TAIJI missions.…”

Section: Introductionmentioning

confidence: 99%

Algorithm for TDI numerical simulation and sensitivity investigation

Wang,

Ni,

Han

et al. 2020

Preprint

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In this work, we introduce a generic algorithm to numerically determine the time delays and spacecraft positions for a time-delay interferometry (TDI) channel in the dynamical case, and streamline the calculations by implementing an SC layout-time delay diagram. We select 11 second-generation TDI channels constructed from four approaches and evaluate their performances including gravitational wave responses, noise levels, and averaged sensitivities under a numerical LISA orbit. The results show that the interference paths of selected TDI channels are well matched and the laser frequency noise should be suppressed under the secondary noise. The channels show various sensitivities in the range of [0.1 mHz, 0.3 Hz], and the major differences appear in the frequency region lower than 20 mHz. The optimal channel A2 or E2 combined from second-generation Michelson TDI channels (X1, X2, and X3) achieves the best sensitivity in the selected channels for the frequency lower than 50 mHz, while the Sagnac α1 channel shows the worse sensitivity. Multiple channels show better sensitivities at some characteristic frequencies compared to the fiducial X1 channel. The Michelson-type channels would have identical sensitivities considering noise level changes with the GW response. The joint A2 + E2 + T2 observation not only enhances the sensitivity of the X1 channel by a factor of √ 2 to 2 but also improves the capacity of sky coverage.

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Orbit design and thruster requirement for various constant arm space mission concepts for gravitational-wave observation

Cited by 13 publications

References 52 publications

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Astrodynamical middle-frequency interferometric gravitational wave observatory AMIGO: Mission concept and orbit design

Revisiting time delay interferometry for unequal-arm LISA and TAIJI

Algorithm for TDI numerical simulation and sensitivity investigation

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