Mars planetary geodesy using earth-based observations of Mars landers

Edwards, C. D.; Kahn, R.; Folkner, W. M.; Preston, R. A.

doi:10.2514/6.1992-4667

Cited by 4 publications

(3 citation statements)

References 14 publications

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“…addition of orbiter and VLBI data may dramatically improve the prospect of detecting the core through its effect on nutations and tidal Love numbers. The timing precision of the X band transponder can be as small as 75 ps if this instrument is properly calibrated[Edwards et al, 1992;Kahn et al, 1996]. However, there may be other limitations such as signal to noise ratio (especially for the lander) which degrades the measurement to about I m under the best of circumstances.…”

mentioning

confidence: 99%

Martian precession and rotation from Viking lander range data

Yoder¹,

Standish²

1997

J. Geophys. Res.

117

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mentioning

confidence: 99%

Martian precession and rotation from Viking lander range data

Yoder¹,

Standish²

1997

J. Geophys. Res.

117

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“…considerably more irregular in longitude than in latitude, in contrast to when it is viewed from Tharsis. Comparing the two configurations, it is apparent that Tharsis is 5.2 times more symmetric than the planet as seen from the pole, which indicates that Tharsis is considerably more axisymmetric than Reasenberg [1977], Kaula [1979], and Kaula et al [1989] also estimated the moment of inertia assuming axisymmetry of Doppler tracking of the future Mars Global Surveyor orbiter [Tyler et al, 1992] and Pathfinder [Edwards et al, 1992' Folkher et al, 1997 (D.A. Paige, personal communication, 1996) lander spacecraft are expected to provide accurate estimates of the position of Mars' rotation pole.…”

Section: Axial Asymmetry Of Tharsismentioning

confidence: 99%

Untitled

1997

J. Geophys. Res.

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The significant power in the Martian gravitational field due to the Tharsis rise may mask or modify gravitational signatures that contain important information on Martian geophysical processes. In order to isolate gravity signals in regions where the field is significantly affected by Tharsis as well to investigate characteristics of the global field, we present a numerical technique to "remove" Tharsis from the Martian gravitational field. Our analysis will show that to first order Tharsis can be represented as a sixth-degree spherical harmonic zonal gravitational feature in a reference frame in which the axis of symmetry runs through the center of the province. We produced the "Mars without Tharsis" (MWT) field by subtracting the gravitational signature of Tharsis from the full field and rotating the spherical harmonics back to the original coordinate system, in which the z-axis is coincident with the planetary rotation axis. Our study yields limits on the moment of inertia factor of 0.361

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“…Kawano et al (1999) investigated the MOP signatures in the Same Beam Interferometry (SBI) observable for two landers (or more) on Mars' surface, providing some analytical expressions of the signatures. A numerical estimation of the MOP precision using a covariance analysis for Earth-based observations of a Martian lander was done by Edwards et al (1992). In this study, we explicitly give the first-order expressions of the signatures for all the MOP and for the lander position in three different observables (Doppler, range and SBI) and we explain the method to derive them.…”

Section: Introductionmentioning

confidence: 99%

Signatures of the Martian rotation parameters in the Doppler and range observables

Yseboodt

Déhant

Péters

2017

Planetary and Space Science

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The position of a Martian lander is affected by different aspects of Mars' rotational motions: the nutations, the precession, the length-of-day variations and the polar motion. These various motions have a different signature in a Doppler observable between the Earth and a lander on Mars' surface. Knowing the correlations between these signatures and the moments when these signatures are not null during one day or on a longer timescale is important to identify strategies that maximize the geophysical return of observations with a geodesy experiment, in particular for the ones on-board the future NASA InSight or ESA-Roscosmos ExoMars2020 missions. We provide first-order formulations of the signature of the rotation parameters in the Doppler and range observables. These expressions are functions of the diurnal rotation of Mars, the lander position, the planet radius and the rotation parameter. Additionally, the nutation signature in the Doppler observable is proportional to the Earth declination with respect to Mars. For a lander on Mars close to the equator, the motions with the largest signature in the Doppler observable are due to the length-of-day variations, the precession rate and the rigid nutations. The polar motion and the liquid core signatures have a much smaller amplitude. For a lander closer to the pole, the polar motion signature is enhanced while the other signatures decrease. We also numerically evaluate the amplitudes of the rotation parameters signature in the Doppler observable for landers on other planets or moons.

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Mars planetary geodesy using earth-based observations of Mars landers

Cited by 4 publications

References 14 publications

Martian precession and rotation from Viking lander range data

Martian precession and rotation from Viking lander range data

Untitled

Signatures of the Martian rotation parameters in the Doppler and range observables

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