Abstract

Volcanoes are key indicators of a planet's internal structure, mechanics, and evolutionary history. Consequently, understanding the types and ages of volcanoes on a planet's surface is an important endeavor. In an attempt to better understand the relationship between morphometry and volcanic processes, we compared low-shield volcanoes on Syria Planum, Mars, with basaltic shields of the eastern Snake River Plain. We used 133 volcanoes on Syria Planum that are covered by Mars Orbiting Laser Altimeter (MOLA) and High Resolution Stereo Camera (HRSC) elevation data and 246 eSRP shields covered by the National Elevation Dataset (NED) for this comparison. Shields on Syria Planum average 191 +/- 88 m tall, 12 +/- 6 km in diameter, 16 +/- 28 km3 in volume, and have 1.7° +/- 0.8 flank slopes. eSRP shields average 83 +/- 44 m tall, 4 +/- 3 km in diameter, 0.8 +/- 2 km3 in volume, and have 2.5° +/- 1 flank slopes. Bivariate plots of morphometric characteristics show that Syria Planum and Snake River Plain low shields form the extremes of the same morphospace shared with some Icelandic olivine tholeiite shields, but are generally distinct from other terrestrial volcanoes. Cluster analysis of Syria Planum and Snake River Plain shields with other terrestrial volcanoes separates these volcanoes into one cluster and the majority of them into the same sub-cluster that is distinct from other terrestrial volcanoes. Principal component and cluster analysis of Syria Planum and Snake River Plain shields using height, area, volume, slope, and eccentricity shows that Syria Planum and Snake River Plain low-shields are similar in shape (slope and eccentricity). Apparently, these low shields formed by similar processes involving Hawaiian-type eruptions of low viscosity (mafic) lavas with fissure controlled eruptions, narrowing to central vents. Initially high eruption rates and long, tube-fed lava flows shifted to the development of small lava lakes that repeatedly overflowed, and on some with late fountaining to form steeper spatter ramparts. However, Syria Planum shields are systematically larger than those on the eastern Snake River Plain. The larger size of Syria Planum shields is likely due to the smaller gravity of Mars, requiring larger magma batches to generate sufficient buoyant force to overcome the strength of rocks in the lithosphere and rise to the surface. Thus, Syria Planum lavas erupt in larger volumes and at higher rates generating larger volcanoes with slightly smaller slopes.

Degree

MS

College and Department

Physical and Mathematical Sciences; Geological Sciences

Rights

http://lib.byu.edu/about/copyright/

Date Submitted

2015-11-01

Document Type

Thesis

Handle

http://hdl.lib.byu.edu/1877/etd8122

Keywords

Volcanism, Mars, Idaho

Included in

Geology Commons

Share

COinS