Domenico Giardini

TL;DR: The GSHAP CAUCAS test area was established under the INTAS Ct.94-1644 (Test Area for sismic Hazard Assessment in the Caucasus) and NATO ARW Ct.95-1521 (Historical and Prehistorical Earthquakes in the Caucasian), with the initial support of IASPEI, UNESCO and ILP.

TL;DR: In 2018, Böse et al. as discussed by the authors used the InSight very-broadband seismometer on the Martian surface to estimate the seismic and noise characteristics observed on Mars.

TL;DR: In this paper, the amplitude, peak frequency, and duration of the seismic signal that would have emanated from this impact were predicted using scaling relationships based on the terrestrial and lunar analogs and numerical modeling.

Abstract: The NASA InSight mission successfully landed on Mars on November 26, 2018 (defined as Sol 0, where sol is the Martian day corresponding to ∼24 h 40 min), in Elysium Planitia. On Sol 25, the lander placed the Seismic Experiment for Interior Structure (SEIS) on the Martian surface. SEIS includes a three-component Very Broadband (VBB) and a three-component Short Period (SP) seismometer (Lognonné et al., 2019). Since Sol 66, SEIS has been covered by the Wind and Thermal Shield (WTS) to minimize atmospheric effects. To complement the seismometer and as a means of characterizing atmospherically induced seismic noise, the Auxiliary Payload Sensor Suite records the surface pressure and also includes the Temperature and Winds for InSight sensors (TWINS) to measure the temperature, wind speed, and wind direction (Lognonné et al., 2019). A description of the initial geophysical observations of the mission can be found in Banerdt et al. (2020), while initial results on seismicity and interior structure are summarized in Giardini et al. (2020); Abstract We present a new class of seismic signals that are recorded by the seismometer placed on the surface of Mars as part of the NASA InSight mission. The signals, termed super high frequency (SF) events, are of short duration (∼20 s), are often similar in amplitude, and feature high-frequency energy between ∼5 and 30 Hz that is dominant on the horizontal components. For detection and characterization of SF events, we employ the available continuous 20 samples per second (sps) data from the Very Broadband instrument. Due to bandwidth limitations, 100 sps data from the short-period sensor are only partially obtainable, but they aid in analysis of the frequency content above 10 Hz and in distinguishing the events from high-frequency noise. From June 2019 to May 2020, 780 SF events have been detected. The events observed occur in repeatable patterns that last for weeks. Initially, the SF events were clustered in the hours before sunset, but more recently, they have been distributed across the evening period. Based on template matching techniques, we have identified 16 distinct families that generally follow the temporal clusters. A thermal origin of these events is suggested, since the majority of the events fall within a ±2 h time window around sunset with extreme temperature changes. The SF events have similarities with thermal events observed on the lunar surface from data collected during the Apollo missions.