Lunar Domes: Properties and Formation Processes by Raffaello Lena, Christian Wöhler, Jim Phillips, Maria Teresa
By Raffaello Lena, Christian Wöhler, Jim Phillips, Maria Teresa Chiocchetta
Lunar domes are constructions of volcanic beginning that are frequently tough to monitor because of their low heights. The Lunar Domes guide is a reference paintings on those elusive positive aspects. It offers a set of pictures for loads of lunar domes, together with telescopic photos obtained with complex yet nonetheless reasonably difficult beginner gear in addition to fresh orbital spacecraft photographs. assorted tools for making a choice on the morphometric houses of lunar domes (diameter, peak, flank slope, edifice quantity) from photo information or orbital topographic information are mentioned. also, multispectral and hyperspectral photograph info are tested, delivering insights into the composition of the dome fabric. a number of category schemes for lunar domes are defined, together with an technique in accordance with the made up our minds morphometric amounts and spectral analyses. additionally, the ebook offers an outline of geophysical versions of lunar domes, which yield information regarding the homes of the lava from which they shaped and the intensity of the magma resource areas under the lunar floor.
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Extra info for Lunar Domes: Properties and Formation Processes
These considerations yield the magma rise speed U according to U= W 2 dp 2τ − . e. not only the magma but also the surrounding rock (“host rock”) is assigned a viscosity value. He shows that the values of W and L are not independent of each other but that their ratio L/W depends on the lava viscosity η. An important model parameter is the ratio p0/G, where p0 denotes the magma pressure diminished by the minimum value of the direction-dependent compressive stress of the crust, and G is the elasticity of the host rock surrounding the dike.
Phillips). b Cross-sectional profile of Kies 2 in east-west direction. The vertical axis is 50 times exaggerated, the curvature of the lunar surface has been subtracted. The height amounts to 55 ± 5 m. e. 9). 11). The dome volume V is computed by integrating the DEM over an area corresponding to a circular region of diameter D around the dome centre. g. due to the presence of shadows cast on the dome surfaces by nearby hills, the volume is estimated based on a cross-section in east-west direction through the centre of the dome, assuming rotational symmetry.
2), Wilson and Head (2003) arrive at a relation for the dike width W which needs to be solved numerically. Notably, both the dike length L and width W are approximately inversely proportional to the magma pressure gradient dp/dz. An important parameter for modelling the geometry of lunar feeder dikes is the vertical pressure gradient dp/dz. Basaltic magmas on the Moon arise from the mantle (Wilson and Head 1996). A classical model of the ascent of lunar magma through the crust is developed by Head and Wilson (1992) and Wilson and Head (1996), who state that the density values of basaltic magma are between those of the mantle and the crust.