th
8
Grade Earth
Science Brookhaven
Academy
Science Question
— What factors
effect lava
flows on Mars?
Why is this question interesting and
important?
—  By studying lava flows on Mars the geology of Mars can be
revealed.
—  This research provides an accurate comparison between
Earth’s features and Mar’s features.
—  By understanding the slope and altitude of a volcano, it can
determine if these factors affect lava flows.
Hypothesis
— If the slope of a volcano is steep, then the
lava will flow more quickly.
— If the lava flow measures short, then the lava
must be more viscous.
Background
—  Olympus Mons, one of the youngest shield volcanoes, is the
largest volcano in the Mars solar system. The lava is sticky
and tears when it moves.
—  Ulysses Patera, buried by Pavonis Mon’s lava, is located at the
middle of Tharsis volcanism. Its striking features are its old
age and the two large impact craters located on it.
—  Ceraunius Tholus is a basaltic shield volcano located in the
Tharsis quadrangle. The slopes are steep with many radial
erosion channels and pitted valleys.
—  Arsia Mons is the southernmost volcano on the Tharsis bulge.
Its name comes from albedo feature, the Roman forest of
Arsia Silva.
Definitions
—  Shield volcanoes- Type of volcano usually built
almost of fluid lava flows
—  Altitude- The height of an object above sea level
—  Slope- Surface of which one end or side is higher than
the other
—  Lava Flows- Streams of molten rock that pour or
ooze from an erupting vent
Definitions
—  Atmosphere- A layer of gases that may surround a
material body of sufficient mass
—  Caldera- A cauldron-like volcanic feature usually
formed by the collapse of land following a volcanic
eruption
—  Olympus Mons- Shield volcano, 14 miles high, tallest
mountain in the solar system, 370 miles wide, the
summit has 6 nested calderas, 2 miles deep
Image of Lava Flows on Mars
—  http://image.mars.asu.edu/scale?
format=jpeg&quality=60&width=400&height=1000&image
=/mars/images/special/themis/iotd/V01028006.png
Lava Flow Formation on Earth
—  Streams of molten rocks ooze from an erupting vent and the lava
cools.
—  The lava flow speed depends on many factors. For example, the
type of lava that erupts and the viscosity of the lava affect the lava
flow pace.
—  When traveling down a steep slope, lava flows are capable of
moving 10 kilometers an hour.
—  Viscous andesite flows move very slowly, and usually do not extend
more than 8 kilometers away from their vents.
—  Because of the lack of information on the formation of lava flows on
Mars, researchers assume the lava flow formations on Mars are very
similar to the lava flow formations on Earth.
Geographic Locations
—  Olympus Mons:
—  Ulysses Patera:
elevation: 22 km
slope: 2-5 degrees
width: 550 km
latitude: 18.4 north
longitude: 226 east
elevation: 2-3 km
slope: 2-7 degrees
width: 2.24 km
latitude: 2.7 north
longitude: 121 west
Geographic Locations
—  Arsia Mons:
—  Ceraunius Tholus:
elevation: 18.1 km
slope: 7 degrees
width: 110 km
latitude: 10 south
longitude: 239 east
elevation: 5.5 km
slope: 8 degrees
width: 130 km
latitude: 24.25 north
longitude: 262 east
Geographic Locations
Olympus Mons
Ulysses Patera
—  elevation: 22 km
—  elevation: 2-3 km
—  slope: 2-5 degrees
—  slope: 2-7 degrees
—  width: 550 km
—  width: 2.24 km
—  latitude: 18.4 north
—  latitude: 2.7 north
—  longitude: 226 east
—  longitude:121 west
Geographic Locations
Arsia Mons
Ceraunius Tholus
—  elevation: 18.1 km
—  elevation: 5.5 km
—  slope: 7 degrees
—  slope: 8 degrees
—  width: 110 km
—  width: 130 km
—  latitude: 10 south
—  latitude:24.25 north
—  longitude: 239 east
—  longitude: 262 east
Experimental Design
—  In this research we will use THEMIS images from Mars
Odyssey
—  We will also use MOLA images found in JMARS
—  This study will focus on lava flows on 4 volcanoes on Mars.
—  Data will be collected to determine if altitude and slope have
any effect on lava flows on Mars
—  Numerous lava flows will be measures on these volcanoes.
Length and width of the lava flow will be used to infer
viscosity of the flow.
Analysis Plan
—  A bar graph will be created to plot height, slope, length and
width of lava flows
—  Using the volcanoes Olympus Mons, Ulysses Paters,
Ceranunius Thollus, and Arsia Mons a graph will be created
of the length and width of multiple lava flows. We will graph
how altitude and slope of these volcanoes effect lava flows
—  Pictures of lava flows will be included.
Websites
—  Mola shaded relief images
—  http://hirise.lpl.arizona.epu/ESP_0185534_1985
—  http://marsprogram.jpl.nasa.gov/gallery/atlas/olympus-
mons.html
—  http://adsaps.harvard.edu
—  http://redplanet.asu.edu/?p=2184
—  http://volcano.oregonstate.edu/oldroot/volcanoes/
planet_volcano/mars/Cones/ulyses.html
—  http://volcanoes.usgs.gov/hazards/lava/index.php
Themis Images
— Many Themis Images are needed
with this research.
Conclusion
—  Science Question:
—  What factors effect lava flows on Mars
—  Hypothesis:
—  If the slope of a volcano is steep, then the lava will flow more quickly.
.
—  If the lava flow measures short, then the lava must be more viscous
—  Importance of Research:
—  Our research project is important to shed light on how slope
and altitude might effect lava flows. The THEMIS camera will
be used to collect data on these factors. By using the camera we
will be able to measure lava flows on our chosen volcanoes.
References
—  Watt, K. (2002). Mars Student Imaging Project: Resource
Manuel. Retrieved January 14, 2013, from Arizona
State University, Mars Student Imaging Project Web
site: http://msip.asu.edu/curriculum.html
—  http://marsed.asu.edu/
—  http://Themis.asu.edu