Scientific objectives of the scientific equipment of the landing platform of the ExoMars-2018 mission

Zelenyǐ, L. M.; Korablev, Oleg; Rodionov, D. S.; Novikov, B.; Marchenkov, K. I.; Andreev, O. N.; Larionov, E. V.

doi:10.1134/s0038094615070229

Cited by 29 publications

(8 citation statements)

References 19 publications

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“…record marsquakes and initiate new discoveries for the years to come, possibly in collaboration with the SEM seismometer on ESA's ExoMars 2020 platform 14 . Arrival time data from two seismometers would provide an additional means to triangulate the location of quakes, and not only lead to more precise locations, but also allow locating more quakes.…”

Section: Insight's Heritage and Challengesmentioning

confidence: 99%

NASA’s InSight mission on Mars—first glimpses of the planet’s interior from seismology

Knapmeyer‐Endrun

Kawamura

2020

Nat Commun

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NASA's InSight mission is the first lander to deploy a seismometer on a planetary body since more than 40 years. With a year of seismic data from Mars, new discoveries on Mars' tectonics and interior structure are just emerging. Aiming at the heart of the planet Unlike all previous Mars missions, which explored the geology, chemistry, and atmosphere of the red planet in great detail, the Interior exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) mission is focused on the interior structure and processes of Mars. It is high time to address these topics as our knowledge of the Martian interior-or, in fact, that of any other terrestrial planet-is poorer than our knowledge for the Earth was 100 years ago. While it is generally assumed that differentiation processes early in the formation of terrestrial planets lead to a subdivision into a brittle rocky crust, a silicate mantle, and an iron-rich core 1 , the finer details are widely uncertain for Mars. This lack of knowledge hampers our understanding of its geodynamic history, and the formation and evolution of terrestrial planets in general. The three experiments carried out by InSight, and specifically the Seismic Experiment for Interior Structure (SEIS), are about to change this. The study of seismic waves generated by earthquakes has been key to our understanding of the internal structure of the Earth and the Moon. For example, detection of signals reflected at the core-mantle boundary resulted in the determination of the Moon's core radius. The thickness of the lunar crust was determined using waves converted at the crust-mantle boundary. On Earth, the absence of direct waves from distances beyond 10,000 km, a so-called shadow zone, led to the discovery of Earth's liquid outer core. Terrestrial seismology nowadays studies 3D fine structure, using 1000 s of seismometers, but on Mars, which was predicted to be seismically active 2 , we still need to answer more basic questions. Current estimates for the average crustal thickness of Mars range from 30 to >100 km 3,4. Accurate estimates of crustal thickness are needed to provide an important constraint on the mantle evolution through time along with the formation of the crust. Crustal thickness directly relates to the mantle's cooling rate, with implications for the style of convection during Mars' early history (i.e., global mantle overturn, stagnant lid convection, or plate tectonics). Gravity and topography constrain relative crustal thickness variations well, but need at least one tie point to obtain absolute values 3. Seismology is the only means for this direct measurement. Mars' mantle may retain compositional layering from its early evolution, which has been destroyed on Earth by vigorous convection. As Mars lacks plate tectonics, but is of sufficient size to have undergone most of the same differentiation processes as early Earth, its mantle structure

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Section: Insight's Heritage and Challengesmentioning

confidence: 99%

NASA’s InSight mission on Mars—first glimpses of the planet’s interior from seismology

Knapmeyer‐Endrun

Kawamura

2020

Nat Commun

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“…In addition, the seismic signals of dust devils may also provide information about the surface and subsurface properties at the InSight landing site by acting as calibration loads (Lorenz et al 2015a(Lorenz et al , 2015b. A Mars microphone is going to be part of the payload of the 2018 Exomars landing platform (Zelenyi et al 2015). The microphone, with a bandwidth of 100 Hz to 10 kHz, will record, for the first time, audio signals at the surface of Mars and is expected to contribute to atmospheric science investigations including dust devil studies (Maurice et al 2016).…”

Section: Marsmentioning

confidence: 99%

Field Measurements of Terrestrial and Martian Dust Devils

Murphy¹,

Steakley²,

Balme³

et al. 2017

Space Sciences Series of ISSI

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“…The infrared-transform spectrometer FAST (Fourier for Atmospheric Species and Temperature) experiment, which will operate on the ExoMars 2022 platform, will play a prominent role at this. The interferometer has an aperture of about 2.5 cm and operates in the spectral range between 1.7 and 17 µm with a best spectral resolution of about 0.05 cm -1 in the Sun tracking mode (Shakun et al, 2019 14 ; Zelenyi et al, 2015 15 ). The instrument is aimed at long-term thermal sounding of the Martian atmosphere and retrieval of the aerosol properties (dust and ice) as well as measurements of minor species by observing the Sun from the surface.…”

Section: Discussionmentioning

confidence: 99%

Martian surface-atmosphere properties obtained with ExoMars infrared instrument TIRVIM and HP3 on InSight

Arnold

Haus

Müller

et al. 2020

Infrared Remote Sensing and Instrumentation XXVIII

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ESA's ExoMars program comprises two missions including the Trace Gas Orbiter (TGO), launched in 2016, and a rover and surface platform, to be launched in 2022. The main scientific objectives of the program are to investigate the Martian environment and climate and search for past or present signs of life. For this purpose, a suite of three infrared spectrometers for remote sensing (Atmospheric Chemistry Suite, ACS) is in use on TGO. One of these instruments is a Fourier transform spectrometer, TIRVIM (Thermal IR V-shape Interferometer Mounting in honor of Vassili Ivanovich Moroz), operating in nadir, limb or solar occultation mode between 1.7 and 17 µm. On ExoMars22's surface platform the spectrometer FAST (Fourier for Atmospheric Species and Temperature) will stu dy the atmosphere and surface at the landing site in the same wavelength range as TIRVIM on TGO. This paper presents the objectives of TIRVIM and FAST. It summarizes selected results of the determination of temperature profiles and dust content in the lower atmosphere of Mars based on radiative transfer modeling of TIRVIM data. Synergetic analyses of TIRVIM spectra and InSight (NASA) in situ measurements of temperature and pressure at InSight's landing site in Elysium Planitia enable improvements of procedures to retrieve parameters from TIRVIM observations. First results on surface temperature obtained from these different data sets together with the measurements to be expected in the future from FAST offer a unique opportunity to compare in situ and IR remote sensing measurements.

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Scientific objectives of the scientific equipment of the landing platform of the ExoMars-2018 mission

Cited by 29 publications

References 19 publications

NASA’s InSight mission on Mars—first glimpses of the planet’s interior from seismology

NASA’s InSight mission on Mars—first glimpses of the planet’s interior from seismology

Field Measurements of Terrestrial and Martian Dust Devils

Martian surface-atmosphere properties obtained with ExoMars infrared instrument TIRVIM and HP3 on InSight

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