Planetary Seismology

Lognonné, Philippe; Johnson, C. L.

doi:10.1016/b978-0-444-53802-4.00167-6

Cited by 85 publications

(118 citation statements)

References 260 publications

(442 reference statements)

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“…As before, the cross-hatched region in Figure 3b shows the parameter space in which Q is satisfied, while k 2 does not provide a tight constraint. Depending on the value of L adopted, temperatures could be anywhere in the range 1420-1650 K. We will argue below that values of L in the range 100-200 km are more likely, in which case temperatures cannot exceed 1525 K. This result is reminiscent of the suggestion made by Lognonne and Mosser [1993] that the bulk Q of Mars can be explained if its mantle is colder than that of the Earth. Figure 2 but assuming the grain size d = 1 mm.…”

Section: Trade-off Between Lid Thickness L and Mantle Temperature T Mmentioning

confidence: 76%

Dissipation at tidal and seismic frequencies in a melt‐free, anhydrous Mars

Nimmo

Faul

2013

JGR Planets

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[1] The measured inward motion of Phobos provides a constraint on the tidal dissipation factor, Q, within Mars. We model viscoelastic dissipation inside a convective Mars using a modified Burgers model based on laboratory experiments on anhydrous, melt-free olivine. The model tidal Q is highly sensitive to the mantle potential temperature and grain size assumed but relatively insensitive to the bulk density and rigidity structure. Q thus provides a tight constraint on the Martian interior temperature. By fitting the observed tidal Q and tidal Love number (k 2 ) values and requiring present-day melt generation, we estimate that for a grain size of 1 cm the current mantle potential temperature is 1625˙75 K, similar to that of the Earth. This estimate is consistent with recent petrologically derived determinations of mantle potential temperature but lower than estimates in some thermal evolution models. The presence of water in the Martian mantle would reduce our estimated temperature. Our preferred mantle grain size of 1 cm is somewhat larger than that of the Earth's upper mantle. The predicted mantle seismic Q is about 130 and is almost independent of depth. The Martian lithosphere represents a high seismic velocity lid, which should be readily detectable with future seismological observations. Citation: Nimmo, F., and U. H. Faul (2013), Dissipation at tidal and seismic frequencies in a melt-free, anhydrous Mars,

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Section: Trade-off Between Lid Thickness L and Mantle Temperature T Mmentioning

confidence: 76%

Dissipation at tidal and seismic frequencies in a melt‐free, anhydrous Mars

Nimmo

Faul

2013

JGR Planets

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“…Increasing values of noise represent mean, 1σ and 3σ noise levels, respectively. The typical thermal noise is assumed to be the 1σ day time values did not work well due to cable issues-see Lognonné and Johnson (2015). It has therefore been evaluated separately from the other thermoelastic contributors.…”

Section: Tether Dilatationmentioning

confidence: 99%

“…The SEIS instrument, see ), De Raucourt et al (2012, Lognonné and Johnson (2015) is an hybrid three-axes seismic instrument. It is composed of a Sensor Assembly (SA) deployed on the ground, and connected to the instrument electronic box located in the spacecraft (E-Box) by an electrical cable referred to as the tether.…”

Section: Seis Instrument Overviewmentioning

confidence: 99%

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The Noise Model of the SEIS Seismometer of the InSight Mission to Mars

et al. 2017

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The SEIS (Seismic Experiment for Interior Structures) instrument on board the InSight mission to Mars is the critical instrument for determining the interior structure of Mars, the current level of tectonic activity and the meteorite flux. Meeting the performance requirements of the SEIS instrument is vital to successfully achieve these mission objectives. The InSight noise model is a key tool for the InSight mission and SEIS instrument requirement setup. It will also be used for future operation planning. This paper presents the analyses made to build a model of the Martian seismic noise as measured by the SEIS seismometer, around the seismic bandwidth of the instrument (from 0.01 Hz to 1 Hz). It includes the instrument self-noise, but also the environment parameters that impact the measurements. We present the general approach for the model determination, the environment assumptions, and we analyze the major and minor contributors to the noise model.

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“…The seismic data obtained on the Moon have contributed to various investigations of the lunar interior (see reviews in Lognonné [2005] and Lognonné and Johnson [2007]). In the early 1980s, all the seismic data obtained by the PSE were compiled and used in investigations of the inner structure model of the Moon [e.g., Goins et al, 1981;Nakamura, 1983].…”

Section: Introductionmentioning

confidence: 99%

Lunar Surface Gravimeter as a lunar seismometer: Investigation of a new source of seismic information on the Moon

et al. 2015

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Lunar seismology has always suffered from the limited number of seismic stations and limited coverage of the seismic network. Additional seismic data are necessary to probe the lunar interior in depth. Instead of a costly new deployment of seismometers, the aim of this study is to investigate the possibility of using the Apollo 17 Lunar Surface Gravimeter (LSG) as a lunar seismometer. The LSG was designed to detect gravitational waves (associated to change in the curvature of spacetime) and tidal ground motion on the Moon, but the data were not investigated for seismic use partially because of a malfunction of the instrument. We first evaluated the influence of the malfunction through comparison with other Apollo seismic data and found that the effect of the malfunction is small, and the LSG detected seismic signals in a manner that was consistent with those of the other Apollo seismometers. Then we carried out source location with the additional station of the LSG. We relocated previously located deep moonquake nests to evaluate the influence of the LSG data, which are generally noisier than other Apollo seismic data. Then we located deep moonquake nests that were previously unlocatable. Forty deep moonquake nests were examined, and we located five new nests. One newly located nest, A284, was most likely to be located on the farside. This series of analyses indicates that the LSG functioned as a lunar seismometer, and that its data are useful for improving seismic analyses with the previous seismic data set of the Moon.

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Planetary Seismology

Cited by 85 publications

References 260 publications

Dissipation at tidal and seismic frequencies in a melt‐free, anhydrous Mars

Dissipation at tidal and seismic frequencies in a melt‐free, anhydrous Mars

The Noise Model of the SEIS Seismometer of the InSight Mission to Mars

Lunar Surface Gravimeter as a lunar seismometer: Investigation of a new source of seismic information on the Moon

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