Numerical simulation of time delay interferometry for a LISA-like mission with the simplification of having only one interferometer

Dhurandhar, S.; Ni, Wei-Tou; Wang, Gang

doi:10.1016/j.asr.2012.09.017

Cited by 31 publications

(42 citation statements)

References 25 publications

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“…For this, we considered all known 492 asteroids with diameter greater than 65 km to obtain an improved ephemeris framework ---CGC 2, and calculated the perturbations due to these 492 asteroids on the ASTROD spacecraft [77]. More recently, we apply different variants of CGC 2 ephemeris framework to study the ASTROD I orbit design/optimization/simulation [78], the ASTROD-GW orbit design/optimization [79], and the numerical Time Delay Interferometry (TDI) for space gravitational-wave mission concepts ASTROD-GW [80], LISA [81] and eLISA [82].…”

Section: Solar System Ephemeridesmentioning

confidence: 99%

Solar-system tests of the relativistic gravity

2017

One Hundred Years of General Relativity

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In 1859, Le Verrier discovered the Mercury perihelion advance anomaly. This anomaly turned out to be the first relativistic-gravity effect observed. During the 157 years to 2016, the precisions and accuracies of laboratory and space experiments, and of astrophysical and cosmological observations on relativistic gravity have been improved by 3-4 orders of magnitude. The improvements have been mainly from optical observations at first followed by radio observations. The achievements for the past 50 years are from radio Doppler tracking and radio ranging together with lunar laser ranging. At the present, the radio observations and lunar laser ranging experiments are similar in the accuracy of testing relativistic gravity. We review and summarize the present status of solar-system tests of relativistic gravity. With planetary laser ranging, spacecraft laser ranging and interferometric laser ranging (laser Doppler ranging) together with the development of drag-free technology, the optical observations will improve the accuracies by another 3-4 orders of magnitude in both the equivalence principle tests and solar-system dynamics tests of relativistic gravity. Clock tests and atomic interferometry tests of relativistic gravity will reach an ever-increasing precision. These will give crucial clues in both experimental and theoretical aspects of gravity, and may lead to answers to some profound issues in gravity and cosmology.

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Section: Solar System Ephemeridesmentioning

confidence: 99%

Solar-system tests of the relativistic gravity

2017

One Hundred Years of General Relativity

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“…Time delay interferometry is considered for ASTROD in 1996 [27,28] and has been worked out for LISA much more thoroughly since 1999. [29,30] In our recent papers, we have worked out various TDI configurations numerically for ASTROD-GW, [31][32][33][34] LISA [35] and eLISA/NGO [36] and compared them with one another. [21] These second generation TDIs all satisfy their respective requirements.…”

Section: Introductionmentioning

confidence: 99%

Orbit optimization and time delay interferometry for inclined ASTROD-GW formation with half-year precession-period

Wang

2015

Chinese Phys. B

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ASTROD-GW (ASTROD [Astrodynamical Space Test of Relativity using OpticalDevices] optimized for Gravitational Wave detection) is a gravitational-wave mission with the aim of detecting gravitational waves from massive black holes, extreme mass ratio inspirals (EMRIs) and galactic compact binaries, together with testing relativistic gravity and probing dark energy and cosmology. Mission orbits of the 3 spacecrafts forming a nearly equilateral triangular array are chosen to be near the Sun-Earth Lagrange points L3, L4 and L5. The 3 spacecrafts range interferometrically with one another with arm length about 260 million kilometers. For 260 times longer arm length, the detection sensitivity of ASTROD-GW is 260 fold better than that of eLISA/NGO in the lower frequency region by assuming the same acceleration noise.Therefore, ASTROD-GW will be a better cosmological probe. In previous papers, we have worked out the time delay interferometry (TDI) for the ecliptic formation. To resolve the reflection ambiguity about the ecliptic plane in source position determination, we have changed the basic formation into slightly inclined formation with half-year precession-period. In this paper, we optimize a set of 10-year inclined ASTROD-GW mission orbits numerically using ephemeris framework starting at June 21, 2035, including cases of inclination angle is 0° (no inclination), 0.5°, 1.0°, 2 1.5°, 2.0°, 2.5° and 3.0°. We simulate the time delays of the first and second generation TDI configurations for the different inclinations, and compare/analyse the numerical results to attain the requisite sensitivity of ASTROD-GW by suppressing laser frequency noise below the secondary noises. To explicate our calculation process for different inclination cases, we take the 1.0° as example to show the orbit optimization and TDI simulation.

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“…where a Newton and a 1PN are the Newtonian and first-order post-Newtonian acceleration from the major celestial bodies in the solar system considered as point mass, a fig is the acceleration due to the figure effects from the Sun, Earth and Moon, and a asteroid is the acceleration from Newtonian perturbation of the 340 asteroids. The explicit interactions in our CGC ephemeris framework are fully described in references [24,36,37]. The thruster needs to provide acceleration a thruster a thruster = a traj  a traj (10) to maintain the constant arm length trajectories.…”

Section: Thruster Accelerationmentioning

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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Numerical simulation of time delay interferometry for a LISA-like mission with the simplification of having only one interferometer

Cited by 31 publications

References 25 publications

Solar-system tests of the relativistic gravity

Solar-system tests of the relativistic gravity

Orbit optimization and time delay interferometry for inclined ASTROD-GW formation with half-year precession-period

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

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