Geological Mapping of the Debussy Quadrangle (H-14) Preliminary Results

Geological mapping of Mercury is crucial to build an understanding of the history of the planet and to set the context for BepiColombo’s observations [1]. Geo-logical mapping of the Debussy quadrangle (H-14) is now underway as part of a program to map the entire planet at a scale of 1:3M using MESSENGER data [2]. The quadrangle is located in the southern hemisphere of Mercury at 0o – 90o E and 22.5o – 65o S. This will be the first high resolution map of the quadrangle as it was not imaged by Mariner 10

Investigating the Martian atmosphere using the ExoMars 2016 lander

Accurate modelling of the Martian atmosphere is essential both for planning and completing future missions to the Martian surface, and for accurate analysis and interpretation of the data that they return. Large dust storms and local wind patterns can affect spacecraft landing profiles, and the level of dust present in the atmosphere may impact lander performance. The ExoMars 2016 Mission will carry an Entry, Descent and Landing Demonstrator Module (EDM), primarily designed to test the ability of ESA’s lander technology to carry a science package to the surface [1]. The Atmospheric Mars Entry and Landing Investigations and Analysis (AMELIA) team [2] will use the module’s entry and descent trajectory to characterise the structure of the atmosphere along the travelled landing profile, and to determine properties of the atmosphere, such as density and wind speed, over a wide altitude range from the upper atmosphere to the surface. Aerosol abundances, including atmospheric dust, will also be characterised. These combined datasets will enable more accurate predictions of the atmospheric environment that future landers will encounter. EDM’s surface science package, DREAMS (Dust characterisation, Risk assessment, and Environment Analyser on the Martian Surface), includes sensors to measure wind speed and direction, surface temperature, pressure, and the amount of atmospheric dust present near the surface [3]. We will use the descent and surface profile data collected by EDM to verify and improve current Martian atmospheric modelling completed at The Open University, using both the global circulation and mesoscale models. [1] Forget et al. (2011) Fourth International Workshop on the Mars Atmosphere: Modeling and Observations, Paris. [2] Ferri et al. (2012) 9th International Planetary Probe Workshop (IPPW9), Toulouse. [3] Esposito et al. (2013) EPSC Abstracts Vol. 8, EPSC2013-815

Stratigraphical evidence of Elysium sea ice from HiRise images

Abstract not available

Icelandic debris flow and their relationship to martian gullies

Abstract not available

Dust devils on Mars: Effects of surface roughness on particle threshold

Abstract not available

Dust devils on Earth and Mars: Extension of particle threshold laboratory simulations

Abstract not available

Regolith-atmosphere water vapour interaction at Gale crater

The exchange of water between the atmosphere and regolith on Mars has been modelled for many decades, but mainly with simplified 1D models, and often with few observations to compare with. Thanks to the Rover Environmental Monitoring Station (REMS) aboard Curiosity, we now have obser-vations of relative humidity at a height of ~1.6 m spanning hundreds of sols. We use a mesoscale model coupled to a subsurface regolith model to study the regolith-atmosphere interaction in and around Gale crater, including atmospheric circulation patterns

The changing trends of childhood poisoning at a tertiary children’s hospital in South Africa

Context. Information on childhood poisoning in the developingworld, including South Africa, is scarce, despite its contribution tomorbidity and mortality.Objective. We describe the profile of children with exposuresand poisonings presenting to Red Cross War Memorial Children’sHospital (RCWMCH) in Cape Town, South Africa, from 2003 to2008 and compare the trends of causative agents over the past twodecades.Methods. Cases were identified by review of the RCWMCH caserecords.Results. Of the total incidents (N=2 872), paraffin (kerosene)was the commonest agent (n=692, 24%) with 124 poisoningsincluding two deaths. Drugs were the most common toxin group(n=988, 34%), including 139 single-drug poisonings with 5deaths; 4 associated with traditional medicine use. Householdcleaning product incidents (n=302, 10%) resulted in 29 singleproductpoisonings with no deaths. Pesticide incidents (n=311,10%) included 6 deaths; 203 (65%) incidents were due toorganophosphates or carbamates. The suburban distribution ofthe main toxin groups varied. Comparing 1987 and 2008, thenumber of incidents decreased from 1 116 to 447; drug and paraffinincidents decreased respectively (from 673 to 150 and from 332 to87), household cleaning products and cosmetics increased (21 to69) and pesticide incidents increased (7 to 69).Conclusion. Despite a decrease in the overall number of incidentsover two decades at RCWMCH, paraffin and drugs remainthe principal agents responsible for paediatric exposures andpoisonings, with increasing incidents due to household cleaningproducts and pesticides. Identification of these toxin groups comingfrom specific suburbs allows for targeted prevention initiatives

Martian Dust Devils: When to Watch for Them

This work investigates surface dust lifting by Martian dust devils within a global-scale computer model, and has revealed unexpected behaviour in the timings of these atmospheric events. This work aims to improve current knowledge of the function played by dust devils in the Martian dust cycle: understanding how dust devils contribute to the dust loading of the Martian atmosphere is key to understanding the planet’s current climate, and to making predictions of the environment that future landers and rovers will encounter