Assessment of Environments for Mars Science Laboratory Entry, Descent, and Surface Operations

Vasavada, A. R.; Chen, Allen; Barnes, J. R.; Burkhart, P. Daniel; Cantor, B. A.; Dwyer-Cianciolo, Alicia M.; Fergason, Robin L.; Hinson, D. P.; Justh, Hilary L.; Kass, D. M.; Lewis, S. R.; Mischna, M. A.; Murphy, James R.; Rafkin, Scot; Tyler, D.; Withers, Paul

doi:10.1007/978-1-4614-6339-9_21

Cited by 19 publications

(29 citation statements)

References 75 publications

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“…The question remains, will these near surface atmosphere improvements to M‐GITM (below 50 km) modify its upper atmosphere structure and dynamics? Recent comparisons of a 1‐D Mars radiative‐convective model [ Vasavada et al , ; Haberle et al , ] and the corresponding 1‐D application of M‐GITM suggest that (a) the incorporation of a PBL scheme in M‐GITM will not likely impact its upper atmosphere and (b) the application of eddy thermal conductivity below 50 km will not impact upper atmosphere temperatures. However, the incorporation of topography will impact upper atmosphere structure and dynamics, as indicated previously Bell et al [].…”

Section: Mars Gitm Simulation Results and Comparisons With Data Setsmentioning

confidence: 99%

Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere

et al. 2015

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A new Mars Global Ionosphere-Thermosphere Model (M-GITM) is presented that combines the terrestrial GITM framework with Mars fundamental physical parameters, ion-neutral chemistry, and key radiative processes in order to capture the basic observed features of the thermal, compositional, and dynamical structure of the Mars atmosphere from the ground to the exosphere (0-250 km). Lower, middle, and upper atmosphere processes are included, based in part upon formulations used in previous lower and upper atmosphere Mars GCMs. This enables the M-GITM code to be run for various seasonal, solar cycle, and dust conditions. M-GITM validation studies have focused upon simulations for a range of solar and seasonal conditions. Key upper atmosphere measurements are selected for comparison to corresponding M-GITM neutral temperatures and neutral-ion densities. In addition, simulated lower atmosphere temperatures are compared with observations in order to provide a first-order confirmation of a realistic lower atmosphere. M-GITM captures solar cycle and seasonal trends in the upper atmosphere that are consistent with observations, yielding significant periodic changes in the temperature structure, the species density distributions, and the large-scale global wind system. For instance, mid afternoon temperatures near ∼200 km are predicted to vary from ∼210 to 350 K (equinox) and ∼190 to 390 k (aphelion to perihelion) over the solar cycle. These simulations will serve as a benchmark against which to compare episodic variations (e.g., due to solar flares and dust storms) in future M-GITM studies. Additionally, M-GITM will be used to support MAVEN mission activities (2014)(2015)(2016).

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Section: Mars Gitm Simulation Results and Comparisons With Data Setsmentioning

confidence: 99%

Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere

et al. 2015

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“…The Mars Regional Atmospheric Modeling System mesoscale model [ Rafkin et al ., ], which has been validated against available observational data [e.g., Vasavada et al . []; Chen et al . []], indicates that turbulent exchange of heat with the atmosphere, particularly at night, contributes very little to changes in the surface ground temperatures.…”

Section: Interpretations and Discussionmentioning

confidence: 99%

Observations and preliminary science results from the first 100 sols of MSL Rover Environmental Monitoring Station ground temperature sensor measurements at Gale Crater

et al. 2014

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We describe preliminary results from the first 100 sols of ground temperature measurements along the Mars Science Laboratory's traverse from Bradbury Landing to Rocknest in Gale. The ground temperature data show long-term increases in mean temperature that are consistent with seasonal evolution. Deviations from expected temperature trends within the diurnal cycle are observed and may be attributed to rover and environmental effects. Fits to measured diurnal temperature amplitudes using a thermal model suggest that the observed surfaces have thermal inertias in the range of 265-375 J m, which are within the range of values determined from orbital measurements and are consistent with the inertias predicted from the observed particle sizes on the uppermost surface near the rover. Ground temperatures at Gale Crater appear to warm earlier and cool later than predicted by the model, suggesting that there are multiple unaccounted for physical conditions or processes in our models. Where the Mars Science Laboratory (MSL) descent engines removed a mobile layer of dust and fine sediments from over rockier material, the diurnal temperature profile is closer to that expected for a homogeneous surface, suggesting that the mobile materials on the uppermost surface may be partially responsible for the mismatch between observed temperatures and those predicted for materials having a single thermal inertia. Models of local stratigraphy also implicate thermophysical heterogeneity at the uppermost surface as a potential contributor to the observed diurnal temperature cycle.

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“…Some fraction of that variation must be due to the crater circulation since the upslope/downslope flows induced by the crater should have an impact on measured surface pressures. While the presence of these flows has yet to be confirmed (Curiosity is not close enough to Mount Sharp or the crater rim to detect them with certainty), a variety of atmospheric models predict that they exist and are quite strong [ Vasavada et al ., ; Tyler and Barnes , ; Haberle et al ., ; Harri et al ., ]. During the day the upslope flow along the slopes of Mount Sharp and the walls of the crater rim exports air from the crater floor lowering overall surface pressures.…”

Section: Observations and Preliminary Interpretationmentioning

confidence: 99%

Preliminary interpretation of the REMS pressure data from the first 100 sols of the MSL mission

et al. 2014

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We provide a preliminary interpretation of the Rover Environmental Monitoring Station (REMS) pressure data from the first 100 Martian solar days (sols) of the Mars Science Laboratory mission. The pressure sensor is performing well and has revealed the existence of phenomena undetected by previous missions that include possible gravity waves excited by evening downslope flows, relatively dust-free convective vortices analogous in structure to dust devils, and signatures indicative of the circulation induced by Gale Crater and its central mound. Other more familiar phenomena are also present including the thermal tides, generated by daily insolation variations, and the CO 2 cycle, driven by the condensation and sublimation of CO 2 in the polar regions. The amplitude of the thermal tides is several times larger than those seen by other landers primarily because Curiosity is located where eastward and westward tidal modes constructively interfere and also because the crater circulation amplifies the tides to some extent. During the first 100 sols tidal amplitudes generally decline, which we attribute to the waning influence of the Kelvin wave. Toward the end of the 100 sol period, tidal amplitudes abruptly increased in response to a nearby regional dust storm that did not expand to global scales. Tidal phases changed abruptly during the onset of this storm suggesting a change in the interaction between eastward and westward modes. When compared to Viking Lander 2 data, the REMS daily average pressures show no evidence yet for the 1-20 Pa increase expected from the possible loss of CO 2 from the south polar residual cap.

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Assessment of Environments for Mars Science Laboratory Entry, Descent, and Surface Operations

Cited by 19 publications

References 75 publications

Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere

Mars Global Ionosphere‐Thermosphere Model: Solar cycle, seasonal, and diurnal variations of the Mars upper atmosphere

Observations and preliminary science results from the first 100 sols of MSL Rover Environmental Monitoring Station ground temperature sensor measurements at Gale Crater

Preliminary interpretation of the REMS pressure data from the first 100 sols of the MSL mission

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