STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

MSIP Proposal Outline

I. Introduction

Which type of crater (preserved or modified) is more common in two specific regions with similar latitudes (Southern Highlands-Nirgal Vallis or Rise)?

This science question is important because it could determine how Mars’ atmosphere and terrain are compared to Earth within similar latitudes (equator region).Our Intro to Geology class has interest in this science question because our results could possibly show the most common locations for meteor impacts and the affect wind erosion plays has on the surface of Mars. Our scope of craters will be those that are 5km or larger within these two regions.

From preliminary observations, there seems to more impact craters within Nirgal Vallis. We hypothesize the following for our two specific regions.

Tharsis Rise-more preserved craters Nirgal Vallis-more modified craters

II. Background

Preserved: Most recent crater Modified: The older crater raised rims & near perfect craters changes by erosion or other impacts

When meteor impacts hit the surface of Mars, the craters are fresh with little to no alteration. While the crater sits on the surface, it is altered with wind which is the dominant process of erosion on Mars. With time, the crater diminishes in size and structure as shown on the figures above. MARS STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

Background continued:

The following diagram displays how craters are formed on the any planet surface due to meteor impact. MARS STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

. In the above THEMIS picture, we observe two preserved craters overlapping in the lower middle section. In the image below, we discovered a large modified crater in the upper left of this THEMIS picture.

MARS STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

Background continued:

The map below is entitled MOLA. The different colors represented determine elevation along the surface of Mars. Our two regions of interest (Tharsis Rise and Nirgal Vallis-Southern Highlands) can be found on opposite sides of . Our specific area of study (latitude and longitude) with reference to both zones will include crater analysis between 0-30 S degrees latitude and 240-330 E longitude.

MARS STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

III. Experiment Design

The specific spacecraft and camera that we will use in order to collect data for our research question is the THEMIS camera aboard Mars Odyssey. The JMARS program will enable us to view archived crater images in specific geographic regions. The regions that we will be focusing on are the Tharsis Rise and Nirgal Vallis within the Southern cratered Highlands. These two areas are separated by Valles Marineris. The amount of THEMIS crater images we will need in order to answer our question is roughly between 100-150. Image identification will allow us and other scientists to reexamine the images. Latitude and longitude will allow us to map where each image we examine is located. Specific feature(s): we will look for are modified and preserved craters.

Procedure:

1.) Examine the images taken by THEMIS camera through JMARS program.

2.) Specify the craters on the images by giving each specific type of crater a color to distinguish them from one another.

3.) Accumulate the amount of modified and preserved craters in both the Tharsis Rise and NirgasValles regions.

4.) Transfer the data to a comprehensible data table and graph.

5.) Re-state hypothesis with findings and summarize results within the conclusion.

IV. Analysis Plan

Our data collection table during our trip at ASU will look similar to this model.

Image ID Latitude Longitude Diameter Type (preserved or Area (Tharsis Rise or modified) Nirgal Vallis)

MARS STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

The following column graph represents a similar graph we as a class will create to display our results. Both modified and preserved craters will be our X axis variable while the # of those we find within our two selected regions will be our Y axis variable.

Y-axis Column Graph

Number of Craters Observed

X-axis 3 Ages of Craters

The MOLA map will display our crater image locations both in the Tharsis Rise and Southern Highlands- Nirgal Vallis. The latitude zone will be 0 to 30 degrees S and the longitude 240-330 degrees E.

MOLA map with plotted crater images

MARS STUDENT IMAGING PROJECT ASU MARS EDUCATION PROGRAM

V. Conclusion

Our class is proposing to answer the following science question while at :

Which type of crater (preserved or modified) is more common in two specific regions with similar latitudes (Southern Highlands-Nirgal Vallis or Tharsis Rise)?

VI. References

Watt, K. (2002). Mars Student Imaging Project: Resource Manuel. Retrieved June 29, 2006, (the date you downloaded) from Arizona State University, Mars Student Imaging Project Web site: http://msip.asu.edu/curriculum.html.

Crater Process Image (Background Section) http://www.google.com/imgres?imgurl=http://www.psi.edu/explorecraters/intro_pic s

THEMIS website www.themis.asu.edu

JMARS interface website www.jmars.asu.edu