Physics Coursework Craters Secondary Data

Hiesinger (2013), Lunar sinuous rilles: Distribution, characteristics, and implications for their origin, Planet.

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Summary We have covered the purpose for this initial post, including the selection of a data set, and determination of a research topic based on the data set.

Additionally, we have determined the content of a personal codebook for the data set based on the topic scope, and formulation of a hypothesis for our research topic. Rothman (2001), Statistics of Mars’ topography from the Mars Orbiter Laser Altimeter: Slopes, correlations, and physical Models, J. Res., 106(E10), 23723–23735, doi:10.1029/2000JE001403.

I am currently in the first week of the first course, Data Management and Visualization.

As part of this first week, I am selecting a research question and data sets that I will continue to work on throughout the course.

Kreslavsky, Lunar Orientale Impact Basin Secondary Craters: Spatial Distribution, Size-Frequency Distribution and Estimation of Fragment Size, Journal of Geophysical Research, submitted.

Head (2017), Evidence for stabilization of the ice-cemented cryosphere in earlier martian history: Implications for the current abundance of groundwater at depth on Mars, Icarus, 288, 120–147, doi:10.1016/j.icarus.20. Links to the study, codebook and data set are in the References section at the bottom of this post.After reviewing the materials, I have decided I am interested in physical characteristics of the craters, specifically diameter (DIAM_CIRCLE_IMAGE) and depth (DEPTH_RIMFLOOR_TOPOG).Alternately I can choose a public data set of my own.I must then provide a topic of interest related to the specific data set.The data sets for the above and earlier studies are not readily available for comparison.However, the Aharonson study does indicate that certain physical characteristics, such as diameter and rim slope have a correlation. Mazarico (2011), A global catalog of large lunar crater (≥20 KM) from the Lunar Orbiter Laser Altimeter, This data includes a more complete assessment of the probable-to-certain impact basins on the surface of Mercury, as well as includes a number of additional craters, particularly in locations where the imaging from the MESSENGER flybys and Mariner 10 observations were not ideal for crater recognition.This 3-D stereo image taken by the Mars Exploration Rover Spirit’s navigation camera shows the rover’s lander and, in the background, the surrounding martian terrain.As rim slope is somewhat related to crater depth, I can hypothesize that crater diameter and depth do have a direct correlation to each other.The degree to which they are related remains unknown at this point until I begin analysis.


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