Constantinos Charalambous

Imperial College London

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Co-Authors

W. T. Pike

Imperial College London

108

Philippe Lognonné

Université Paris Cité

106

W. B. Banerdt

Jet Propulsion Laboratory

102

Domenico Giardini

ETH Zurich

John Clinton

ETH Zurich

Anna Horleston

University of Bristol

Simon C. Stähler

ETH Zurich

Savas Ceylan

ETH Zurich

Taïchi Kawamura

Institut de physique du globe de Paris

Alexander Stott

Université de Toulouse

Cooperative Institutions

Jet Propulsion Laboratory

157

Centre National de la Recherche Scientifique

California Institute of Technology

ETH Zurich

Institut de physique du globe de Paris

Planetary Science Institute

Centre National d'Études Spatiales

Université Paris Cité

Sorbonne Université

Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR)

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InSight seismic data from Mars: Effect and treatment of transient data disturbances

AGU Fall Meeting Abstracts (2020)

John‐Robert Scholz Rudolf Widmer‐Schnidrig Paul D. Davis Philippe Lognonné Baptiste Pinot

Transient (computer programming)

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InSight Short Period Seismometers Detection of Dust Devils on Mars

Lunar and Planetary Science Conference (2019)

T. Warren W. T. Pike Alexander Stott J. M. McClean Constantinos Charalambous

Seismometer

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SEIS first year: nm/s^2 (and less) broadband seismology on Mars and first steps in Mars-Earth-Moon comparative seismology.

AGU Fall Meeting Abstracts (2019)

Philippe Lognonné W. B. Banerdt W. T. Pike Domenico Giardini D. Banfield

InSight is the first planetary mission with a seismometer package, SEIS, since the Apollo Lunar Surface Experiments Package. SEIS is complimented by APSS, which has as a goal to document the atmospheric source of seismic noise and signals. Since June 2019, SEIS has been delivering 6 axis 20 sps continuous seismic data, a rate one order of magnitude larger originally planned. More than 50 events have been detected by the end of July 2019 but only three have amplitudes significantly above the SEIS instrument requirement. Two have clear and coherent arrivals of P and S waves, enabling location, diffusion/attenuation characterization and receiver function analysis. The event’s magnitudes are likely ≤ 3 and no clear surface waves nor deep interior phases have been identified. This suggests deep events with scattering along their final propagation paths and with large propagation differences as compared to Earth and Moon quakes. Most of the event’s detections are made possible due to the very low noise achieved by the instrument installation strategy and the very low VBB self-noise. Most of the SEIS signals have amplitudes of spectral densities in the 0.03-5Hz frequency bandwidth ranging from 10-10 m/s2/Hz1/2 to 5 10-9 m/s2/Hz1/2. The smallest noise levels occurs during the early night, with angstrom displacements or nano-radian tilts. This monitors the elastic and seismic interaction of a planetary surface with its atmosphere, illustrated not only by a wide range of SEIS signals correlated with pressure vortexes, dust devils or wind activity but also by modulation of resonances above 1 Hz, amplified by ultra-low velocity surface layers. After about one half of a Martian year, clear seasonal changes appear also in the noise, which will be discussed. One year after landing, the seismic noise is therefore better and better understood, and noise correction techniques begun to be implemented, either thanks to the APSS wind and pressure sensors, or by SEIS only data processing techniques. These data processing techniques open not only the possibility of better signal to noise ratio of the events, but are also used for various noise auto-correlation techniques as well as searches of long period signals. Noise and seismic signals on Mars are therefore completely different from what seismology encountered previously on Earth and Moon.

Seismometer

Microseism

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Array-based seismic measurements of OSIRIS-REx's re-entry

EarthArXiv (California Digital Library) (2024)

Benjamin Fernando Constantinos Charalambous N. C. Schmerr Timothy Craig Jonathan Wolf

The return home of the OSIRIS-REx spacecraft in September 2023 marked only the fifth time that an artificial object entered the Earth's atmosphere at interplanetary velocities. Although rare, such events serve as valuable analogues for natural meteoroid re-entries; enabling study of hypersonic dynamics, shockwave generation, and acoustic-to-seismic coupling. Here, we report on the signatures recorded by a dense (100-m scale) 11-station array located almost directly underneath the capsule's point of peak atmospheric heating in northern Nevada. Seismic data are presented which allow inferences to be made about the shape of the shockwave's footprint on the surface, the capsule's trajectory, and its flight parameters.

Osiris

Footprint

10.31223/x51d7h

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MODIFICATION OF HOMESTEAD HOLLOW AT THE INSIGHT LANDING SITE

Abstracts with programs - Geological Society of America (2019)

J. A. Grant N. H. Warner C. M. Weitz M. P. Golombek Sharon A. Wilson

10.1130/abs/2019am-334535

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Active tectonics on Mars as seen by InSight

Lunar and Planetary Science Conference (2020)

Simon C. Stähler John Clinton Domenico Giardini S. Smrekar Maren Böse

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Seismic activity rate of Mars, based on 420 Sols of InSight data

Simon C. Stähler Martin Knapmeyer Domenico Giardini John Clinton W. T. Pike

<p>We present an updated estimate of the seismic activity rate of Mars after seven months of high-quality recording of the InSight SEIS instrument. The instrument has been deployed fully on Sol 60 (February 2, 2019) and has been recording with excellent performance since then. The first distant marsquake was observed on Sol 105 (March 14), the first local event on Sol 128 (April 7). From then until early January 2020 (Sol 400), 23 likely events and another 13 candidate events have been observed. Due to a strong diurnal variation in background noise and the generally low magnitude of the activity (compared to Earth), events have been observed only in few low-noise periods of the day. The change of seasons varied the duration of these low-noise periods over the mission, with a magnitude and time-dependent effect on detectability of events and the quantitative estimation of event rates and moment release.</p><p>We present a statistical analysis of the global seismic activity level based on a preliminary seismic magnitude model, weighted by the temporal evolution of the ambient noise over half a Martian year. The resulting number of events smaller magnitude 3 is roughly consistent with the pre-mission estimate of Golombek (1992) and the medium model of Knapmeyer et al. (2006), however, as of now, there is a statistically significant lack of events above magnitude 3.5. This hints at a distribution that is skewed towards smaller events, compared to terrestrial global averages.</p>

Moment magnitude scale

10.5194/egusphere-egu2020-13482

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Constraints for the Martian Crustal Structure From Rayleigh Waves Ellipticity of Large Seismic Events

Geophysical Research Letters (2023)

Sebastián Carrasco Brigitte Knapmeyer‐Endrun Ludovic Margerin Zongbo Xu Rakshit Joshi

Abstract For the first time, we measured the ellipticity of direct Rayleigh waves at intermediate periods (15–35 s) on Mars using the recordings of three large seismic Martian events, including S1222a, the largest event recorded by the InSight mission. These measurements, together with P‐to‐s receiver functions and P‐wave reflection times, were utilized for performing a joint inversion of the local crustal structure at the InSight landing site. Our inversion results are compatible with previously reported intra‐crustal discontinuities around 10 and 20 km depths, whereas the preferred models show a strong discontinuity at ∼37 km, which is interpreted as the crust‐mantle interface. Additionally, we support the presence of a shallow low‐velocity layer of 2–3 km thickness. Compared to nearby regions, lower seismic wave velocities are derived for the crust, suggesting a higher porosity or alteration of the whole local crust.

Classification of discontinuities

Rayleigh Wave

Discontinuity (linguistics)

10.1029/2023gl104816

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Seismic Noise Polarization as a Measure of Wind Direction and Speed by Correlating InSight SEIS/APSS Observations on Mars

N. A. Teanby Robert Myhill Anna Horleston James Wookey W. T. Pike

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Rock Size-frequency Distributions of the InSight Landing Site, Mars

M. P. Golombek Allyson R. Trussell N. R. Williams Constantinos Charalambous H. Abarca

Earth and Space Science Open Archive This work has been accepted for publication in Earth and Space Science. Version of RecordESSOAr is a venue for early communication or feedback before peer review. Data may be preliminary. Learn more about preprints. preprintOpen AccessYou are viewing the latest version by default [v2]Rock Size-frequency Distributions of the InSight Landing Site, MarsAuthorsMatthew P.GolombekiDAllyson R.TrusselliDNathan RobertWilliamsiDConstantinosCharalambousiDHallieAbarcaNicholas HaleWarnerMargaretDeahnMarshall R.TrautmanBobCroccoiDJohn A.GrantiDErnstHauberiDRobert GDeeniDSee all authors Matthew P. GolombekiDCorresponding Author• Submitting AuthorCalifornia Institute of Technology/JPLiDhttps://orcid.org/0000-0002-1928-2293view email addressThe email was not providedcopy email addressAllyson R. TrusselliDCalifornia Institute of TechnologyiDhttps://orcid.org/0000-0002-7113-8782view email addressThe email was not providedcopy email addressNathan Robert WilliamsiDJet Propulsion LabiDhttps://orcid.org/0000-0003-0602-484Xview email addressThe email was not providedcopy email addressConstantinos CharalambousiDImperial College LondoniDhttps://orcid.org/0000-0002-9139-3895view email addressThe email was not providedcopy email addressHallie AbarcaJet Propulsion Laboratoryview email addressThe email was not providedcopy email addressNicholas Hale WarnerSUNY Geneseoview email addressThe email was not providedcopy email addressMargaret DeahnSUNY Geneseoview email addressThe email was not providedcopy email addressMarshall R. TrautmanJet Propulsion Laboratory, Caltechview email addressThe email was not providedcopy email addressBob CroccoiDJet Propulsion Laboratory, CaltechiDhttps://orcid.org/0000-0002-5397-6475view email addressThe email was not providedcopy email addressJohn A. GrantiDSmithsonian InstitutioniDhttps://orcid.org/0000-0001-8276-1281view email addressThe email was not providedcopy email addressErnst HauberiDDLRiDhttps://orcid.org/0000-0002-1375-304Xview email addressThe email was not providedcopy email addressRobert G DeeniDJet Propulsion LaboratoryiDhttps://orcid.org/0000-0002-5693-641Xview email addressThe email was not providedcopy email address

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10.1002/essoar.10507665.2

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