Question - Arizona State University
Transcript of Question - Arizona State University
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Question
• Which volcano on the Tharsis region of Mars is the youngest?
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Importance
• We believe that this question is important and interesting because we don’t have any evidence of recent tectonic activity on Mars. Therefore, we were interested in which volcano is the youngest.
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Hypotheses
• Our main hypotheses, the volcano on the Tharsis Region that is youngest is Pavonis Mons.
• Our alternative hypotheses, the volcano on the Tharsis Region that is youngest is Olympus Mons.
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Definitions
• Volcano-A volcano is an opening, or rupture in a planet’s surface or crust, which allows hot magma, volcanic ash, and gases to escape from below the surface.
• Crater-A basin resulting from the collision of an object with a planetary surface. (Made by meteorites)
Citation: class notes
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Themis image of volcano • There is no image I.D. • Olympus Mons is the largest volcano on Mars.
• It is about as large as the state of Arizona. • It has four to six visible craters on the top. (not 46, 4 to 6)
h#p://marsprogram.jpl.nasa.gov/gallery/atlas/olympus-‐mons.html
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THEMIS IMAGE OF CRATER
• The image I.D. of this crater is V07993020 • This crater was most likely created by a large
meteorite • It seems to be about as wide as the several craters
on top of Olympus Mons.
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VOLCANO FORMATION • Volcanoes on Earth are created from a weak spot in the
crust where molten material from the asthenosphere (mantle) comes to the surface. They are found on plate boundaries that are diverging or in subduction zones around the edges of the oceans.
• Volcanoes on Mars were formed in a similar fashion as Earth’s. Except the one shown below and the rest of the volcanoes on the Tharsis region are a shield volcano and those are found in the middle of the plate.
Olympus Mons (left) Mt. Saint Helens (right) Cita9on: class notes
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Crater Formation • Craters on Earth were formed my meteorite impacts. • Craters on Mars were also created my meteorite impact. The reason
why Mars has so many craters is because Mars doesn’t have the same atmosphere as we do, so it isn’t protected like Earth is.
A crater on Mars (left)
Barringer Crater (Right)
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Science Research • The Mariner 9 image of Olympus Mons is one of the first images to show
that Mars has large volcanoes. • THEMIS image of lava flows. Note the lobate shape of the edges. Volcanic
activity, or volcanism, has played a significant role in the geologic evolution of Mars. Scientists have known since the Mariner 9 mission in 1972 that volcanic features cover large portions of the Martian surface. These features include extensive lava flows, vast volcanic plains, and the largest known volcanoes in the Solar System. Martian volcanic features range in age from Noachian (>3.7 billion years) to late Amazonian (< 500 million years), indicating that the planet has been volcanically active throughout its history and probably still is so today.
• When scientists analyzed the ages and chemical composition of several ... Believe it or not, "recent" in geological terms can actually mean "180 million years young. ... To the Tharsis region, home to Olympus Mons, the largest volcano in our ... come from volcanic regions on Mars ? their ages are as young as 180 million ...
• http://en.wikipedia.org/wiki/Volcanology_of_Mars
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Procedures 1. On JMARS (MSIP) software, type in following coordinates: 244E, 7.812. 2. Make a 7x14 data table with following labels: Image I.D. #, Latitude, Longitude, preserved
craters, Modified craters, Destroyed craters, region. 3. Magnify onto volcanic feature that you will collect data on. 4. Click “add new layer”. 5. Go to “MSIP” in first category box. 6. Click on “stamps”. 7. Click on “THEMIS”. 8. Click “set Lon/Lat to bounds of view”. 9. Click “okay” (blue overlapped boxes should appear). 10. Click on a box (should turn yellow). 11. Right click and click on “view THEMIS stamps”. 12. Click on “web browse (image I.D. #)”. 13. Find info table (located at the right- hand side). 14. Copy and paste image I.D. #, longitude, and latitude in to data table made earlier. 15. Count number of preserved, modified, and destroyed. 16. Record data in data table. 17. Repeat steps 2-16 for each volcano.
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Spacecraft and Camera Used
• Spacecraft- the Odyssey • Camera- THEMIS (thermal emission
imaging system)
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Geologic features • We’ll be focusing on geologic
features such as volcanoes and craters. We will study this because our science question asks which volcano in the Tharsis region on Mars is the youngest. We’ll use THEMIS images of craters on the volcanoes and see which volcano has the most and the least which will show the age by using the technique of super positioning.
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Geographic regions
• We’ll be focusing on the Tharsis region of Mars. The Tharsis region holds some of Mars’ largest volcanoes.
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THEMIS Images
• We used 59 THEMIS images to answer our science question.
Olympus Mons
Arsia Mons
Pavonis Mons
Ascraeus Mons
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Column names of data table
• Image I.D. # • Latitude • Longitude • # of preserved craters • # of modified craters • # of destroyed craters • Region ( all of them will state Tharsis since
that is our main focus)
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Measurements
• THE ONLY MEASURING WE’LL BE DOING IS COUNTING THE NUMBER OF CRATERS ON EACH THEMIS IMAGE. THIS IS THE ONLY WAY OF RESEARCHING OUR QUESTION USING THEMIS IMAGES.
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Ascraeus Mons Data Table
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Image ID # La*tude Longitude Preserved Craters
Modified Craters
Destroyed Craters
Region
V26937030 11.405907 253.76805 15 2 1 Tharsis
V17777019 11.396997 254.34744 150 2 2 Tharsis
V41486003 12.340611 254.45581 12 0 0 Tharsis
V26051009 10.718286 254.1094 25 1 0 Tharsis
V19312020 12.99556 254.96169 8 3 1 Tharsis
V45268014 12.113349 256.8067 9 12 2 Tharsis
V05546023 11.094465 256.26218 18 2 0 Tharsis
Continued
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Image ID # La*tude Longitude Preserved Craters
Modified Craters
Destroyed Craters
Region
V25728003 -‐8.06292 238.41304 13 0 0 Tharsis
V34262002 -‐7.705117 237.16313 8 3 1 Tharsis
V18078003 -‐7.37774 237.73502 11 2 2 Tharsis
V42361003 -‐10.058286 237.57123 3 2 0 Tharsis
V31904003 -‐8.851785 240.11969 250 2 1 Tharsis
V36396002 -‐8.323527 241.38252 6 2 1 Tharsis
V37856001 -‐8.638034 242.84215 3 2 2 Tharsis
V16755003 -‐7.724043 242.19498 12 3 1 Tharsis
Arsia Mons Data Table
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Image ID # La*tude Longitude Preserved Craters
Modified Craters
Destroyed Craters
Region
V27138002 -‐10.892619 240.79674 6 2 1 Tharsis
V17379001 -‐11.234431 241.20654 4 1 0 Tharsis
V40801003 -‐10.470305 241.3511 5 2 0 Tharsis
V16755004 -‐11.114345 241.73778 11 2 1 Tharsis
V18290003 -‐10.29354 241.80913 26 2 0 Tharsis
V18265002 -‐7.94486 243.30635 4 2 2 Tharsis
V27088003 -‐8.870664 243.56337 5 2 1 Tharsis
Continued
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Olympus Mons Data Table Image ID #
La*tude Longitude Preserved Craters
Modified Craters
Destroyed Craters
Region
V04461003 18 227 2 0 0 Tharsis
V18377009 18 227 1 0 0 Tharsis
V04848015 17.259539 226.58228 5 0 0 Tharsis
V08543016 17.467382 227.64622 25 15 0 Tharsis
V04461003 19.16305 227.01256 20 25 0 Tharsis
V26052010 17.520014 226.20972 15 10 0 Tharsis
V11351008 18.349787 225.8119 20 10 0 Tharsis
V06321015 17.417927 226.98459 15 10 0 Tharsis
V27225040 17.509874 225.91606 15 10 5 Tharsis
V28086021 17.078766 226.27505 10 15 6 Tharsis
V42036009 18.57207 228.8494 15 10 7 Tharsis
V10702005 17.246044 227.17497 25 15 0 Tharsis
V26052010 17.520014 226.20972 15 15 12 Tharsis
V28086021 17.078766 226.27505 20 10 0 Tharsis
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Pavonis Mons data table Image ID #
La*tude Longitude Preserved Craters
Modified Craters
Destroyed Craters
Region
V12386009 1.830684 246.81087 7 15 8 Tharsis
V17615024 1.606787 246.28279 12 12 7 Tharsis
V11450010 1.196657 247.63454 5 10 7 Tharsis
V15743004 0.326678 247.59819 15 6 8 Tharsis
V27636035 0.724564 246.41652 17 10 20 Tharsis
V14258014 1.266217 245.18036 4 0 2 Tharsis
V15169007 0.722308 245.78075 31 20 10 Tharsis
V01639008 0.425045 247.363 3 10 20 Tharsis
V27062043 2.394495 246.32822 15 20 20 Tharsis
V41324003 2.256716 246.54724 20 16 30 Tharsis
V18551012 2.344226 245.58382 9 7 10 Tharsis
V04660006 1.520217 245.91081 5 5 10 Tharsis
V27063001 -‐0.397498 245.95433 12 10 15 Tharsis
V19412011 -‐0.815804 248.52803 6 10 10 Tharsis
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Crater Data Graph
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-‐90
-‐60
-‐30
0
30
60
90
0 30 60 90 120 150 180 210 240 270 300 330 360
Latitude
Longitude
Mola Map
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Conclusion (part 1)
• Our scientific question was: which volcano on the Tharsis region of Mars is the youngest?
• Our main hypothesis was: the volcano on the Tharsis Region that is youngest is Pavonis Mons.
• Our alternative hypotheses was: the volcano on the Tharsis Region that is youngest is Olympus Mons
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Conclusion (part 2)
• We believe that this question is important and interesting because we don’t have any evidence of recent tectonic activity on Mars. Therefore, we were interested in how old the youngest volcano is.
• The evidence was how many craters were found on each volcano. We found a reasonable amount to support our hypothesis.
• The possible noise we could have made was that we could have miscounted the amount of craters on each volcano in the Tharsis region and this could lead to incorrect data tables.
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Conclusion (part 3)
• Our hypothesis was proven to be wrong by the data that we collected. The volcano on the Tharsis Region that is youngest is Ascraeus Mons, was proved to be supported in our experiment. Ascraeus Mons ended up having 309 craters in all. The volcano that had the largest amount was actually the one that we thought that would be the youngest, Pavonis Mons. Pavonis Mons had 489 craters. We say the volcano that has the least amount of craters would be the youngest because it makes sense that the longer the volcano has been around, the more craters it would have.
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References • h#p://themis.asu.edu/
• h#p://marsed.mars.asu.edu/msip-‐home
• h#p://www.geology.sdsu.edu/how_volcanoes_work/mars.html
• h#p://www.astrobio.net/pressrelease/4723/the-‐history-‐of-‐volcanism-‐on-‐mars
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End of Presentation, thank you for watching!