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  • Lunar and Planetary Science and Exploration  (45)
  • Meteorology and Climatology  (4)
  • Space Sciences (General); Lunar and Planetary Science and Exploration  (1)
  • 11
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    Age of Martian Impact Crater Lakes: The Morphological Evidence for Recent Lacustrine Activity (2000)
    In:  Other Sources
    Details
    Publication Date: 2017-10-02
    Description: Some impact crater lakes could be as recent as Middle Amazonian, which raises a number of critical questions about their generation processes. We discuss the geological evidence and the possibility of a contribution from meteorological control.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXI; LPI-Contrib-1000
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  • 12
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    GCM Simulations of Tropical Ice Accumulations: Implications for Cold-based Glaciers (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-11
    Description: Each of the three Tharsis Montes shield volcanoes on Mars has fan-shaped deposits on their flanks. A detailed analysis of the multiple facies of the Arsia Mons deposits, coupled with field observations of polar glaciers in Antarctica, shows that they are consistent with deposition from cold-based mountain glaciers. Key features of these glaciers are: (1) they formed only on the western flank of each volcano, (2) enough ice accumulated to cause them to flow but without basal melting, (3) there were multiple advances and retreats, (4) the last major glaciation was more than several million years ago, (5) the areal extent of the deposits they left behind decreases northward, (6) together the deposits range in elevation from a low of 1.5 to a high of 8.5 km, and (7) there are no signs that significant accumulation is occurring today.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXV: Mars Polar Science and Exploration; LPI-Contrib-1197
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  • 13
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    Reconciling the MOLA, TES, and Neutron Observations of the North Polar CO2 Mass Budget on Mars (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: There are now three independent observations of the CO2 polar cap mass budget of Mars' north polar cap. The first is based elevation changes detected by the Mars Orbiter Laser Altimeter (MOLA) on the Mars Global Surveyor (MGS). The second is based on MGS Thermal Emission Spectrometer (TES) broadband observations of the solar and infrared radiation fields at the top of the atmosphere. The third is based on neutron counts measured by the neutron spectrometer (NS) on Odyssey. The TES data are based on an energy balance. The net radiative loss (gain) in a column is balanced by latent heating due condensation (sublimation) of CO2. In calculating the mass budget, the other main energy sources, atmospheric heat transport and subsurface conduction, were neglected. At the pole, atmospheric heat transport is indeed a small term. However, subsurface heat conduction can be significant because at the North Pole water ice, which has a high thermal conductivity compared to bare soil, is a dominant component of the subsurface. Thus, heat conducted down into the ice during summer will slowly bleed back out during fall and winter reducing the amount of CO2 that condenses on the pole. We have taken a first cut at quantifying this effect by fitting a curve to Paige's estimates of the conducted energy flux in his analysis of Viking IRTM data.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Third International Conference on Mars Polar Science and Exploration; LPI-Contrib-1184
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  • 14
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    Carbon Dioxide Convection in the Martian Polar Night and Its Implications for Polar Processes (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: Each Martian year nearly 30% of the atmosphere is exchanged with the polar ice caps. This exchange occurs through a combination of direct surface condensation and atmospheric precipitation of carbon dioxide. It has long been thought the amount of condensation within the polar night is maintained by a balance between diabatic processes such as radiative cooling and latent heating from condensing CO2. This assumption manifests itself in Mars General Circulation Models (GCM) in such a way as to never allow the atmospheric temperature to dip below the saturation temperature of CO2. However, observations from Mars Global Surveyor (MGS) Radio Science (RS) and the Thermal Emission Spectrometer (TES) have demonstrated this assumption to be, at best, approximate. Both RS and TES observations within the polar nights of both poles indicate substantial supersaturated regions with respect to CO2. The observed temperature profiles suggest conditionally unstable regions containing planetary significant amounts of potential convective energy. Presented here are estimates of the total planetary inventory of convective available potential energy (CAPE) and the potential convective energy flux (PCEF). The values for CAPE and PCEF are derived from RS temperature profiles and compared to Mars GCM results using a new convective CO2 cloud model that allows for the formation of CAPE.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Third International Conference on Mars Polar Science and Exploration; LPI-Contrib-1184
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  • 15
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    Outflow Channels Influencing Martian Climate: Global Circulation Model Simulations with Emplaced Water (2005)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: The existence of surface water on Mars in past geologic epochs is inferred on the basis of geomorphologic interpretation of spaceflight images, and is supported by the recent Mars Odyssey identification of ice-rich soils [1]. The Mars Exploration Rovers have provided further chemical evidence for past surface hydrologic activity [2]. One issue is whether this water-rich climate ever existed in a steady state, or whether it was triggered by catastrophic events such as large impacts [3], and/ or catastrophic outburst floods, the topic of consideration here.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 18; LPI-Contrib-1234-Pt-18
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  • 16
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    Obliquity Driven Climate Change in Mars' Recent Past (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: Mars has a natural mechanism for experiencing significant climate change and redistributing surface ice. Obliquity changes alone are quite capable of moving ice into low latitudes and may provide an explanation for the many geological landforms that strongly indicate recent climate change.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Third International Conference on Mars Polar Science and Exploration; LPI-Contrib-1184
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  • 17
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    3D Simulations of the Early Mars Climate with a General Circulation Model (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: The environmental conditions that existed on Mars during the Noachian period are subject to debate in the community. In any case, there are compelling evidence that these conditions were different than what they became later in the amazonian and possibly the Hesperian periods. Indeed, most of the old cratered terrains are disected by valley networks (thought to have been carved by flowing liquid water), whereas younger surface are almost devoid of such valleys. In addition, there are evidence that the erosion rate was much higher during the early noachian than later. Flowing water is surprising on early Mars because the solar luminosity was significantly lower than today. Even with the thick atmosphere (up to several bars).To improve our understanding of the early Mars Climate, we have developed a 3D general circulation model similar to the one used on current Earth or Mars to study the details of the climate today. Our first objective is to answer the following questions : how is the Martian climate modified if 1) the surface pressure is increased up to several bars (our baseline: 2 bars) and 2) if the sun luminosity is decreased by 25 account the heat possibly released by impacts during short periods, although it may have played a role .For this purpose, we have coupled the Martian General Circulation model developed at LMD with a sophisticated correlated k distribution model developped at NASA Ames Research Center. It is a narrow band model which computes the radiative transfer at both solar and thermal wavelengths (from 0.3 to 250 microns).
    Keywords: Lunar and Planetary Science and Exploration
    Type: Third International Conference on Mars Polar Science and Exploration; LPI-Contrib-1184
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  • 18
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    Interannual Atmospheric Variability Simulated by a Mars GCM: Impacts on the Polar Regions (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: It is often assumed that in the absence of year-to-year dust variations, Mars weather and climate are very repeatable, at least on decadal scales. Recent multi-annual simulations of a Mars GCM reveal however that significant interannual variations may occur with constant dust conditions. In particular, interannual variability (IAV) appears to be associated with the spectrum of atmospheric disturbances that arise due to baroclinic instability. One quantity that shows significant IAV is the poleward heat flux associated with these waves. These variations and their impacts on the polar heat balance will be examined here.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Third International Conference on Mars Polar Science and Exploration; LPI-Contrib-1184
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  • 19
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    Water-Ice Clouds in the LMDs Martian General Circulation Model (2003)
    In:  CASI
    Details
    Publication Date: 2017-10-02
    Description: The interest for Martian water ice clouds has recently taken a new extent given their likely involvement both in climate and in the hydrological cycle. Previous related microphysical studies have already discussed the complex interactions between airborne dust and clouds [2]. Whereas water ice mantles upon dust cores enhance sedimentation rates and thus possibly change the vertical distribution of dust and water, the advection of clouds by winds could also modulate the geographical distribution of volatiles. Within this context, only 3D modeling based on the use of Martian General Circulation Models (MGCM) is able to give us a consistent clue of the global climatic aspects of Martian clouds.
    Keywords: Meteorology and Climatology
    Type: Sixth International Conference on Mars; LPI-Contrib-1164
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  • 20
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    History and Progress of GCM Simulations on Recent Mars Climate Change (2004)
    In:  CASI
    Details
    Publication Date: 2018-06-11
    Description: The Mars Global Surveyor and Odyssey spacecraft reveal evidence that Mars may have experienced significant climate change in the recent past (105-106 Myr ago). Examples include gullies [1], cold-based tropical glaciers [2], paleolakes [3], and youthful near-surface ice [4]. Except for the gullies, the evidence for recent climate change requires ice and/or liquid water at low latitudes. An obvious question, therefore, is how is it possible for ice and/or liquid water to exist at low latitudes which is not possible in the present climate system? There are several mechanisms to consider. An episode of intense volcanic activity could alter the mean composition of the atmosphere and, therefore, the climate system. Impacts, depending on the size, composition, and velocity of the impactor are another way to dramatically alter the climate system. Polar wander and solar variability are also possibilities. However, the most promising way to change the climate is through changes in orbital properties. Mars, because of its proximity to Jupiter and lack of a large stabilizing moon, experiences much greater changes in its orbit properties than the Earth.
    Keywords: Meteorology and Climatology
    Type: Lunar and Planetary Science XXXV: Special Session: Mars Climate Change; LPI-Contrib-1197
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