Laser and radio tracking for planetary science missions—a comparison

Dirkx, Dominic; Procházka, Ivan; Bauer, Sven; Visser, Pieter; Noomen, R.; Gurvits, L. I.; Vermeersen, Bert

doi:10.1007/s00190-018-1171-x

Cited by 27 publications

(27 citation statements)

References 87 publications

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“…The stability performance of the unstabilised version on the 2.2 km link shows an order of magnitude improvement over the typical operational performance of ground to space two-way X-band systems at the same integration time (Dirkx et al, 2018).…”

Section: Discussionmentioning

confidence: 89%

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Methods for coherent optical Doppler orbitography

Dix-Matthews

Schediwy

Gozzard

et al. 2020

J Geod

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Doppler orbitography uses the Doppler shift in a transmitted signal to determine the orbital parameters of satellites including range and range-rate (or radial velocity). We describe two techniques for atmosphericlimited optical Doppler orbitography measurements of range-rate. The first determines the Doppler shift directly from a heterodyne measurement of the returned optical signal. The second aims to improve the precision of the first by suppressing atmospheric phase noise imprinted on the transmitted optical signal. We demonstrate the performance of each technique over a 2.2 km horizontal link with a simulated in-line velocity Doppler shift at the far end. A horizontal link of this length has been estimated to exhibit nearly half the total integrated atmospheric turbulence of a vertical link to space. Without stabilisation of the atmospheric effects, we obtained an estimated range rate precision of 17 µm s −1 at 1 s

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Section: Discussionmentioning

confidence: 89%

“…This one-way system determines the range rate (or radial velocity) of the satellite at uncertainties of <0.4 mm s −1 (Moreaux et al, 2019). Typical operational ground to space X-band radio tracking techniques can now achieve precisions at around 20 µm s −1 to 100 µm s −1 after 60 s of integration (Dirkx et al, 2018).…”

mentioning

confidence: 99%

Methods for coherent optical Doppler orbitography

Dix-Matthews

Schediwy

Gozzard

et al. 2020

J Geod

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“…Depending on the dynamics type, multiple formulations for the governing equations may be used, such as Cartesian, Keplerian and Modified Equinoctial Elements for translational dynamics, and quaternions or modified Rodrigues parameters, in combination with angular velocities, for rotational dynamics. States may be propagated in a single-arc or multi-arc fashion, as well as a combination of the two, as described by (Dirkx et al, 2018).…”

Section: Discussionmentioning

confidence: 99%

“…Tudat is applicable to a broad range of topics, and has been used for, among others, simulations of solar system dynamics (Dirkx et al, 2018), interplanetary trajectory design (Musegaas, 2013), planetary system dynamics (Kumar et al, 2015;Dirkx et al, 2016), space debris impact predictions (Ronse and Mooij, 2014) and atmospheric re-entry (Dirkx and Mooij, 2014).…”

Section: Appendix a Relations Between Rotation Representationsmentioning

confidence: 99%

“…Simulation models for various astrometric and radiometric data types are available, and applied by e.g. Dirkx et al ( , 2016Dirkx et al ( , 2017Dirkx et al ( , 2018, with recent publications focussing on the JUICE-PRIDE radio tracking experiment (Gurvits et al, 2013). Models for the detailed analysis of real radio and optical data are currently under development.…”

Section: Appendix a Relations Between Rotation Representationsmentioning

confidence: 99%

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Propagation and estimation of the dynamical behaviour of gravitationally interacting rigid bodies

Dirkx

Mooij

Root

2019

Astrophys Space Sci

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Next-generation planetary tracking methods, such as interplanetary laser ranging (ILR) and same-beam interferometry (SBI) promise an orders-of-magnitude increase in the accuracy of measurements of solar system dynamics. This requires a reconsideration of modelling strategies for the translational and rotational dynamics of natural bodies, to ensure that model errors are well below the measurement uncertainties.The influence of the gravitational interaction of the full mass distributions of celestial bodies, the so-called figure-figure effects, will need to be included for selected future missions. The mathematical formulation of this problem to arbitrary degree is often provided in an elegant and compact manner that is not trivially relatable to the formulation used in space geodesy and ephemeris generation. This complicates the robust implementation of such a model in operational software packages. We formulate the problem in a manner that is directly compatible with the implementation used in typical dynamical modelling codes: in terms of spherical harmonic coefficients and Legendre polynomials. An analytical formulation for the associated variational equations for both translational and rotational motion is derived.We apply our methodology to both Phobos and the KW4 binary asteroid system, to analyze the influence of figure-figure effects during estimation from next-generation tracking data. For the case of Phobos, omitting these effects during estimation results in relative errors of 0.42% and 0.065% for theC 20 andC 22 spherical harmonic gravity field coefficients, respectively. These values are below current uncertainties, but orders of magnitude larger than those obtained from past simulations for accurate tracking of a future Phobos lander, showing the need to apply the methodology outlined in this manuscript for selected future missions.

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Is there a semi-molten layer at the base of the lunar mantle?

Walterová

Běhounková

Efroimsky

2022

Preprint

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Parameterised by the Love number k 2 and the tidal quality factor Q, and inferred from lunar laser ranging (LLR), tidal dissipation in the Moon follows an unexpected frequency dependence often interpreted as evidence for a highly dissipative, melt-bearing layer encompassing the core-mantle boundary. Within this, more or less standard interpretation, the basal layer's viscosity is required to be of order 10 15 to 10 16 Pa.s and its outer radius is predicted to extend to the zone of deep moonquakes. While the reconciliation of those predictions with the mechanical properties of rocks might be challenging, alternative lunar interior models without the basal layer are said to be unable to fit the frequency dependence of tidal Q. The purpose of our paper is to illustrate under what conditions the frequency-dependence of lunar tidal Q can be interpreted without the need for deep-seated partial melt. Devising a simplified lunar model, in which the mantle is described by the Sundberg-Cooper rheology, we predict the relaxation strength and characteristic timescale of elastically-accommodated grain boundary sliding in the mantle that would give rise to the desired frequency dependence. Along with developing this alternative model, we test the traditional model with basal partial melt; and we show that the two models cannot be distinguished from each other by the available selenodetic measurements. Additional insight into the nature of lunar tidal dissipation can be gained either by measurements of higher-degree Love numbers and quality factors or by farside lunar seismology.

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Laser and radio tracking for planetary science missions—a comparison

Cited by 27 publications

References 87 publications

Methods for coherent optical Doppler orbitography

Methods for coherent optical Doppler orbitography

Propagation and estimation of the dynamical behaviour of gravitationally interacting rigid bodies

Is there a semi-molten layer at the base of the lunar mantle?

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