Aerial Seismology Using Balloon-Based Barometers

Krishnamoorthy, Siddharth; Kassarian, Ervan; Martire, Léo; Sournac, A.; Cadu, A.; Lai, Voon Hui; Komjáthy, A.; Pauken, Michael; Cutts, J. A.; Garcia, Raphaël; Mimoun, David; Jackson, Jennifer M.; Bowman, Daniel

doi:10.1109/tgrs.2019.2931831

Cited by 30 publications

(17 citation statements)

References 41 publications

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“…Particularly on Mars, it may allow the remote investigation of meteor entries (Williams, 2001) and related impacts (Daubar et al, 2018), as well as possible nearby landslides, rockfalls, or ejecta falls. Based on terrestrial analogues, one can also reasonably expect acoustic signals from spacecraft entry (Garcés et al, 2004;Yamamoto et al, 2011), the seismo-acoustic coupling of marsquakes (Krishnamoorthy et al, 2018(Krishnamoorthy et al, , 2019Martire et al, 2018), dust devils (Bedard, 2005;Lorenz & Christie, 2015;Tatom et al, 1995), wind-mountain interactions (Larson et al, 1971), and atmospheric turbulence (Howe, 2002).…”

Section: Introductionmentioning

confidence: 99%

Martian Infrasound: Numerical Modeling and Analysis of InSight's Data

et al. 2020

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Acoustic waves in planetary atmospheres couple into the solid surface, producing ground displacements that can be measured using seismometers. On 26 November 2018, the InSight mission successfully landed on Mars. Its objectives include studying Mars' interior using the seismometer SEIS (Seismic Experiment for Interior Structures) and the atmosphere through the weather station APSS (Auxiliary Payload Sensor Suite). Because InSight is the first mission capable of studying infrasound on Mars, we investigate the signature of infrasound both in terms of air pressure and ground velocities. Using numerical simulations, we characterize (1) the acoustic propagation pattern in Martian dusk and (2) the mechanical atmosphere‐to‐ground coupling under acoustic waves. Then, using SEIS data, we demonstrate that two low‐frequency monotone events (S0133a and S0189a) are in fact infrasound trapped in the atmospheric nocturnal surface waveguide. We base our demonstration on the following facts. (1) Seismic signals rarely produce, at a given station, a single frequency varying from one event to the other. (2) No clear seismic phases have been identified for such events. (3) The observed SEIS signals present the characteristics expected for trapped infrasound observed through their compliance effects (specific frequency response, more energy on the vertical component, ±90° phase shift between vertical and horizontal components, and no detection on pressure sensor at these low amplitude levels). Our simulations of the nocturnal waveguide's response are however subject to uncertainties because (1) it relies on the sol‐to‐sol variability of the atmosphere, and (2) subsurface properties are not properly known at this time.

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Section: Introductionmentioning

confidence: 99%

Martian Infrasound: Numerical Modeling and Analysis of InSight's Data

et al. 2020

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“…Numerous geophysical events were already accurately modelled, such as the generation of seismically induced infrasound (Krishnamoorthy et al 2018;Martire et al 2018;Krishnamoorthy et al 2019;Garcia et al 2021), or the conversion of pressure perturbations to ground motion (Martire et al 2020). In general, both large-scale and small-scale phenomena can be modelled, as well as atmospheric sources or surface-induced atmospheric perturbations.…”

Section: O N C L U S I O Nmentioning

confidence: 99%

SPECFEM2D-DG, an open-source software modelling mechanical waves in coupled solid–fluid systems: the linearized Navier–Stokes approach

Martire

Martin

Brissaud

et al. 2021

Geophysical Journal International

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Summary We introduce SPECFEM2D-DG, an open-source, time-domain, hybrid Galerkin software modeling the propagation of seismic and acoustic waves in coupled solid-fluid systems. For the solid part, the visco-elastic system from the routinely used SPECFEM2D software is used to simulate linear seismic waves subject to attenuation. For the fluid part, SPECFEM2D-DG includes two extensions to the acoustic part of SPECFEM2D, both relying on the Navier-Stokes equations to model high-frequency acoustics, infrasound, and gravity waves in complex atmospheres. The first fluid extension, SPECFEM2D-DG-FNS, was introduced in 2017 by Brissaud, Martin, Garcia, and Komatitsch; it features a non-linear Full Navier-Stokes (FNS) approach discretised with a discontinuous Galerkin numerical scheme. In this contribution, we focus only on introducing a second fluid extension, SPECFEM2D-DG-LNS, based on the same numerical method but rather relying on the Linear Navier-Stokes (LNS) equations. The three main modules of SPECFEM2D-DG all use the Spectral Element Method (SEM). For both fluid extensions (FNS and LNS), two-way mechanical coupling conditions preserve the Riemann problem solution at the fluid-solid interface. Absorbing outer boundary conditions (ABCs) derived from the Perfectly Matched Layers’ (PML) approach are proposed for the LNS extension. The SEM approach supports complex topographies and unstructured meshes. The LNS equations allow the use of range-dependent atmospheric models, known to be crucial for the propagation of infrasound at regional scales. The LNS extension is verified using the method of manufactured solutions, and convergence is numerically characterized. The mechanical coupling conditions at the fluid-solid interface (between the LNS and elastodynamics systems of equations) are verified against theoretical reflection-transmission coefficients. The ABCs in the LNS extension are tested and prove to yield satisfactory energy dissipation. In an example case study, we model infrasonic waves caused by quakes occurring under various topographies; we characterize the acoustic scattering conditions as well as the apparent acoustic radiation pattern. Finally, we discuss the example case and conclude by describing the capabilities of this software. SPECFEM2D-DG is open-source and is freely available online on GitHub.

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“…Indeed, the DAVINCI (Deep Atmosphere of Venus Investigation of Noble Gases, Chemistry, and Imaging) and VERITAS (Venus Emissivity, Radio science, InSAR, Topography, And Spectroscopy) missions (Garvin et al, 2020;Smrekar et al, 2020), recently selected for flight in the ninth NASA Discovery mission competition, as well as EnVision (de Oliveira et al, 2018), announced in June 2021 as the winner of ESA's fifth Medium-class competition, include a focus on volcanic activity among their science objectives. And recent work to develop airborne infrasound sensors may enable aerial-platform-based studies of volcanic infrasound at Venus through seismic detection (Brissaud et al, 2021;Krishnamoorthy et al, 2018Krishnamoorthy et al, , 2019.…”

Section: Rationale For This Studymentioning

confidence: 99%

“…In addition, aerial platforms that follow the wind would naturally find themselves in a direction preferred by acoustic waves traversing an atmospheric duct. Thus, the detection of volcanic activity through seismic and infrasound monitoring on the surface on a long-lived lander (Kremic et al, 2017), in its atmosphere on a balloon (Brissaud et al, 2021;Krishnamoorthy et al, 2019Krishnamoorthy et al, , 2020, or on an airglow-monitoring orbiter such as the Venus Airglow Measurements and Orbiter for Seismicity (VAMOS) concept (Sutin et al, 2018), are all complementary methods by which ongoing or fresh eruption events might be detected and characterized.…”

Section: The Prospect For Detecting Eruptions On Venusmentioning

confidence: 99%

Estimates on the Frequency of Volcanic Eruptions on Venus

Byrne

Krishnamoorthy

2022

JGR Planets

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There is little question that Venus is a volcanic world-that is, that the second largest rocky planet in the Solar System has hosted major volcanic activity, and its surface is composed predominantly of volcanic materials. When the Soviet Union's Venera 8 landed on the Venus surface, the spacecraft returned compositional data pointing to a silicic rock type at that landing site (Vinogradov et al., 1973). Alkaline and tholeiitic basaltic compositions, respectively, were found at the landing sites of the Venera 13 and 14 missions (Surkov et al., 1983), suggesting that much of the surface of Venus is predominantly basaltic (although Vega 2 lander measurements pointed to an anorthosite-norite-troctolite composition at its landing site: Surkov et al., 1985). Venera 13 and 14 also returned color images from the surface, revealing a landscape of thinly stratified rocks consistent with lithified accumulations of volcanic ash or sediment (Bazilevskii et al., 1983;Byrne et al., 2020).The NASA Magellan mission ultimately yielded the first high-resolution (∼100 m/pixel) global radar image mosaic of the planet, as well as altimetric and emissivity datasets (e.g., Saunders et al., 1990), and showed Venus to be a world with discernable lava flows, major rift zones, thousands of shield volcanoes (Crumpler et al., 1993), and domes and shield fields (i.e., volcanic fields) (Ivanov & Head, 2013), as well as a range of volcanotectonic landforms including arachnoids, novae, calderas, and distinctive, quasi-circular corona structures that feature high degrees of localized (and generally extensional) strain (Stofan et al., 1992). The planet also has a dearth of impact craters less than 25 km in diameter and none less than 3 km across (Phillips et al., 1991). Crater statistics derived

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Aerial Seismology Using Balloon-Based Barometers

Cited by 30 publications

References 41 publications

Martian Infrasound: Numerical Modeling and Analysis of InSight's Data

Martian Infrasound: Numerical Modeling and Analysis of InSight's Data

SPECFEM2D-DG, an open-source software modelling mechanical waves in coupled solid–fluid systems: the linearized Navier–Stokes approach

Estimates on the Frequency of Volcanic Eruptions on Venus

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