Mars: An Introduction to its Interior, Surface and Atmosphere (Cambridge Planetary Science)
Language: English
Pages: 286
ISBN: 1107644879
Format: PDF / Kindle (mobi) / ePub
Our knowledge of Mars has changed dramatically in the past 40 years due to the wealth of information provided by Earth-based and orbiting telescopes, and spacecraft investigations. Recent observations suggest that water has played a major role in the climatic and geologic history of the planet. This textbook covers our understanding of the planet's formation, geology, atmosphere, interior, surface properties, and potential for life. This interdisciplinary textbook encompasses the fields of geology, chemistry, atmospheric sciences, geophysics, and astronomy. Each chapter introduces the necessary background information to help the non-specialist understand the topics explored. It includes results from missions through 2006, including the latest insights from Mars Express and the Mars Exploration Rovers. Containing the most up-to-date information on Mars, this textbook is essential reading for graduate courses, and an important reference for researchers.
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Tends to suppress the formation of plagioclase. Also, Mars is larger than the Moon and pressures near the base of the magma ocean could produce majorite and garnet phases, which will sequester the aluminum that would otherwise form a plagioclase-rich crust (Borg and Draper, 2003; Elkins-Tanton et al., 2003; Agee and Draper, 2004). The depth of the martian magma ocean is not well constrained. Righter et al. (1998) used isotopic abundances in melt inclusions from the martian meteorites to estimate.
Of the Olympia Planitia dunes indicates smaller particles than sand and likely originates from erosion of a sulfur-rich volcanic layer within the adjacent polar layered deposits (Herkenhoff and Vasavada, 1999; Byrne and Murray, 2002; Langevin et al., 2005a). Smaller deposits of saltated material form sand dunes. Crescent-shaped barchan dunes (Figure 5.33a) form when the wind blows consistently from one direction. Transverse dunes (Figure 5.33b) are the most common dune morphology on Mars. They.
Within Galle Crater, near 52.3°S 329.9°E. Image is ∼4 km across. (MOC image MOC2-1494, NASA/ JPL/ MSSS.) (c) This distributary fan in Eberswalde Crater (24.0°S 33.7°W) displays features suggestive of fluvial deposition within this crater. (MOC image MOC2-1225a, NASA/JPL/MSSS.) NADBARLO: 9780521852265c05 7/11/07 56:46:51pm page 152 153 Geologic processes (e) (d) Figure 5.40 (cont.) January 1997 October 1996 Mars North Polar Cap March 1997 HST . WFPC2 PRC97-15b • ST Scl OPO • May 20,.
Image from 4 September 2001. (Image STScIPRC01-31, NASA/Cornell/SSI/STScI/AURA.) Figure 6.7 White clouds can be seen over the Tharsis volcanoes and western Valles Marineris in this MOC regional view. Orographic clouds commonly occur near the tall martian volcanoes. (MOC image MOC2-144, NASA/JPL/MSSS.) global in extent, depending on the atmospheric conditions. Global dust storms (Figure 6.6) typically occur near perihelion when it is summer in the southern hemisphere. The stronger daytime.
2003. As of mid-2006, Odyssey’s THEMIS and GRS instruments continue to return data. The two Mars Exploration Rover (MER) missions, named Spirit and Opportunity, were sent to Mars in 2003 to investigate sites which might contain evidence of ancient water and the early martian climate. Spirit was launched on 10 June 2003, with Opportunity following on 7 July. Both rovers utilized the airbag-cushion landing NADBARLO: 9780521852265c01 7/11/07 16:59:22pm page 13 14 Introduction to Mars Figure 1.6.