Thesis (Ph. D.)--Ohio State University, 2004. / Document formatted into pages; contains xvi, 158 p. Includes bibliographical references. Abstract available online via OhioLINK's ETD Center; full text release delayed at author's request until 2005 Sep. 20.

The Penn-State/NCAR MM5 mesoscale model was adapted for mesoscale simulations of the Martian atmosphere (the OSU MMM5). The NASA Ames Mars GCM provides initial and boundary conditions. High-resolution maps for albedo, thermal inertia and topography were developed from Mars Global Surveyor (MGS) data; these baseline maps are processed to appropriate resolutions for use in the GCM and the mesoscale model. The OSU MMM5 is validated in Chapter 2 by comparing with surface meteorology observed at the Viking Lander 1 (VL1) and Mars Pathfinder (MPF) landing sites. How the diurnal cycle of surface pressure (the surface pressure tide) is affected by boundaries, domain/nest choices and the resolution of surface properties (topography, albedo and thermal inertia) is examined. Chapter 2 additionally shows the influence of regional slope flows in the diurnal surface pressure cycle for certain locations on Mars. Building on the methods of Chapter 2, Chapter 3 describes the northern midsummer polar circulation and the circulations (both large and small scale) that influence it. Improvements to the model for these studies include: the topographical gradient is now considered when computing surface insolation, and the thermal inertia maps and model initialization are improved for high latitudes; this yields a realistic simulation of surface temperatures for the North Pole Residual Cap (NPRC) and the surrounding region. The midsummer polar circulation is vigorous, with abundant and dynamically important transient eddies. The preferred locations of transients varies significantly during this study, between L[subscript s]=l20 and L[subscript s]=l50. At L[subscript s]=l20 transient circulations are seen primarily along the NPRC margin, consistently producing strong flow over the residual cap (~l5 m/s). By L[subscript s]=135, transient eddies form a "storm track" between the northern slopes of Tharsis and the NPRC. By L[subscript s]=150, the circulation is becoming strong and winter-like. These transient eddies may be important in the Martian annual water cycle; many of the observed circulations are poorly (or not) simulated in present day Mars GCMs. Increased resolution and polar stereographic domains provide improvement over GCMs for high latitude studies of atmospheric circulations. These results are in agreement with recent observations. Future work includes model refinements and water vapor transport studies. / Graduation date: 2005

Thesis (M.Sc.)--York University, 2007. Graduate Programme in Earth and Space Science. / Typescript. Includes bibliographical references (leaves 119-121). Also available on the Internet. MODE OF ACCESS via web browser by entering the following URL: http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&res_dat=xri:pqdiss&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&rft_dat=xri:pqdiss:MR38822

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Thesis (M.S.)--University of Hawaii at Manoa, 2008. / Includes bibliographical references (leaves 208-234). / xiv, 234 leaves, bound ill. (some col.) 29 cm

Report (M. Eng.)--Virginia Polytechnic Institute and State University, 1991. / Vita. Abstract. Includes bibliographical references (leaves 75-76). Also available via the Internet.

Undergraduate honors paper--Mount Holyoke College, 2006. Dept. of Astronomy. / Includes bibliographical references (leaves 80-87).

Thesis (Ph. D.)--University of Texas at Austin, 2006. / Vita. Includes bibliographical references.

Typescript (photocopy). / Digitized by Kansas Correctional Industries

The European Space Agency's ExoMars 2020 mission gives the astrobiology community the opportunity to scrutinise instrumentation, landing sites and proposed biosignatures in preparation for this mission. A miniaturised Raman spectrometer will be included as part of the payload instrumentation. The main focus of this work is to test the capabilities of this technique in support of this mission. The impact crater environment is one of the most valuable targets in search for life on Mars. One of the most well preserved craters on earth has evidence of microbial life in the post-impact hydrothermal deposits and the surface mineral crusts. Raman spectroscopy is able to identify more habitable forms of sulphate and detect photo-protective microbial pigments in the crusts. One of the building blocks of life is organic carbon. Raman spectroscopy will primarily be used to characterise organics, and as Mars has a limited atmosphere and lacks a global magnetic field, the surface of Mars is heavily oxidised. The effect that oxidation has on the Raman carbon signal is therefore important. Results show that hematite has an interfering band at the same frequency as the carbon D band, which could result in a misinterpretation of the carbon order, so caution must be taken. Oxidised iron could be a viable energy source of iron-reducing bacteria. One of the most common reduction morphologies in the geological record is the reduction spheroid. They are most likely formed by iron-reducing bacteria, and could be used as a biosignature on Mars. Results show that Raman spectroscopy is able to detect reduction spheroids by tracking the presence of hematite. Experimental work aiming to simulate the formation of a reduction spheroid was unsuccessful but shed light on the complexity of crystalline Fe(III) reduction. This work has highlighted the capabilities and limitations of Raman spectroscopy prior to the ExoMars mission.