Free bodily vibrations of the terrestrial planets

Bolt, Bruce A.; Derr, John S.

doi:10.1016/0083-6656(69)90005-1

Cited by 22 publications

(4 citation statements)

References 61 publications

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“…Normal modes were therefore an early proposal as the ideal way to obtain the internal structure of Mars with a single station (e.g. Bolt and Derr 1969), and discussed again by papers published during the design phase of Viking and Mars96 respectively (Okal and Anderson 1978;Lognonné and Mosser 1993). The instruments finally delivered for these two missions nevertheless lacked sufficient long period response to observe normal modes.…”

Section: Normal Modes and Tidesmentioning

confidence: 99%

Planned Products of the Mars Structure Service for the InSight Mission to Mars

et al. 2016

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The InSight lander will deliver geophysical instruments to Mars in 2018, including seismometers installed directly on the surface (Seismic Experiment for Interior Structure, SEIS). Routine operations will be split into two services, the Mars Structure Service (MSS) and Marsquake Service (MQS), which will be responsible, respectively, for defining the structure models and seismicity catalogs from the mission. The MSS will deliver a series of products before the landing, during the operations, and finally to the Planetary Data System (PDS) archive. Prior to the mission, we assembled a suite of a priori models of Mars, based on estimates of bulk composition and thermal profiles. Initial models during the mission will rely on modeling surface waves and impact-generated body waves independent of prior knowledge of structure. Later modeling will include simultaneous inversion of seismic observations for source and structural parameters. We use Bayesian inversion techniques to obtain robust probability distribution functions of interior structure parameters. Shallow structure will be characterized using the hammering of the heatflow probe mole, as well as measurements of surface wave ellipticity. Crustal scale structure will be constrained by measurements of receiver function and broadband Rayleigh wave ellipticity measurements. Core interacting body wave phases should be observable above modeled martian noise levels, allowing us to constrain deep structure. Normal modes of Mars should also be observable and can be used to estimate the globally averaged 1D structure, while combination with results from the InSight radio science mission and orbital observations will allow for constraint of deeper structure

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Section: Normal Modes and Tidesmentioning

confidence: 99%

Planned Products of the Mars Structure Service for the InSight Mission to Mars

et al. 2016

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“…Despite the challenges presented by the effective deployment of a LP seismometer and the expected lack of very large‐magnitude marsquakes, normal mode detection was always an ultimate goal for Mars seismology. This was listed in descriptions of the first Mars seismic exploration projects (Bolt & Derr, 1969; Okal & Anderson, 1978) and remained in most later ones (Gudkova & Zharkov, 1996; Lognonné et al., 1996, 2000; Lognonné & Mosser, 1993) including InSight (Bissig et al., 2018; Lognonné et al., 2019; Lognonné & Johnson, 2015; Panning et al., 2017).…”

Section: Introductionmentioning

confidence: 99%

Detection of Mars Normal Modes From S1222a Event and Seismic Hum

Lognonné

Schimmel²,

Stutzmann

et al. 2023

Geophysical Research Letters

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The inversion of normal mode eigenfrequencies is one of the most efficient ways to determine the physically averaged interior structure of a planet, as illustrated by Dziewonski and Anderson (1981), one of the most cited references in seismology. On Earth, normal mode observations require both large quakes, with magnitude larger than 7, and well-shielded, long-period (LP), low-noise seismic instrumentation (Laske & Widmer-Schnidrig, 2015). This delayed the first observation of Earth normal modes until the great M w = 9.5 Chile earthquake in 1960, several decades after the body wave hodochrone table determined by Jeffreys (1937). See Benioff et al. (1961), Lognonné andClévédé (2002), Laske and Widmer-Schnidrig (2015), among others for reviews of Earth's normal modes.Despite the challenges presented by the effective deployment of a LP seismometer and the expected lack of very large-magnitude marsquakes, normal mode detection was always an ultimate goal for Mars seismology. This was listed in descriptions of the first Mars seismic exploration projects (

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“…Thus, determining Mars' normal modes has been proposed as one of the overarching goals of a seismological mission to Mars from the early times of space exploration (Kovach and Anderson 1965;Bolt and Derr 1969) to Viking (Okal and Anderson 1978) as well as the more recent projects such as Mesur (Solomon et al 1991), Intermarsnet (Lognonné et al 1996) and NetLander (Lognonné and Giardini 2000). Several papers detail detection techniques have been detailed in several papers (Lognonné and Mosser 1993;Zharkov and Gudkova 1997;Gudkova and Zharkov 2004;Lognonné 2005;Johnson 2007, 2015).…”

Section: Introductionmentioning

confidence: 99%

Mars’ Background Free Oscillations

et al. 2019

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Observations and inversion of the eigenfrequencies of free oscillations constitute powerful tools to investigate the internal structure of a planet. On Mars, such free oscillations can be excited by atmospheric pressure and wind stresses from the Martian atmosphere, analogous to what occurs on Earth. Over long periods and on a global scale, this phenomenon may continuously excite Mars' background free oscillations (MBFs), which constitute the so-called Martian hum. However, the source exciting MBFs is related both to the global-scale atmospheric circulation on Mars and to the variations in pressure and wind at the planetary boundary layer, for which no data are available. To overcome this drawback, we focus herein on a global-scale source and use results of simulations based on General Circular Models (GCMs). GCMs can predict and reproduce long-term, global-scale Martian pressure and wind variations and suggest that, contrary to what happens on Earth, daily correlations in the Martian hum might be generated by the solar-driven GCM. After recalling the excitation terms, we calculate MBFs by using GCM computations and estimate the contribution to the hum made by the global atmospheric circulation. Although we work at the lower limit of MBF signals, the results indicate that the signal is likely to be periodic, which would allow us to use more efficient stacking theories than can be applied to Earth's hum. We conclude by discussing the perspectives for the InSight SEIS instrument to detect the Martian hum. The amplitude of the MBF signal is on the order of nanogals and is therefore hidden by instrumental and thermal noise, which implies that, provided the predicted daily coherence in hum excitation is present, the InSight SEIS seismometer should be capable of detecting the Martian hum after monthly to yearly stacks.

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Free bodily vibrations of the terrestrial planets

Cited by 22 publications

References 61 publications

Planned Products of the Mars Structure Service for the InSight Mission to Mars

Planned Products of the Mars Structure Service for the InSight Mission to Mars

Detection of Mars Normal Modes From S1222a Event and Seismic Hum

Mars’ Background Free Oscillations

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