lab 4 report filled out Astronomy

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Cratering and the Martian Surface 10/16/2022 Dating Volcanic Activity 1. Over the last billion years, there have been 10 times fewer 500+meter impact craters than 250+ meter ones, and 10 times more 63+ meter than 250+ meter ones. 2. A billion-year old surface should have 1000 times more 125+ meter impact craters than a million-year old surface. 3. The density curves for the smallest size craters are flat between four and one billion years, because there were so many impact events at that time that you couldn't incur one without rubbing out a former crater. Is the same trend true for 250+ and 500+ meter craters, and if not, why not? No the trend is not true for 250+ and 500+ meter craters. The 250+ and 500+ meter craters start getting bigger and start taking the place of other smaller craters 4. Hadriaca Patera Mark all craters equal to or larger than 500 meters in diameter , and then use your measurement of the crater surface density and Figure 4.5 to derive an age for this surface. Justify your final answer, by showing your work for each stage of the problem and describing your intermediate results. There are 9 craters measuring.038 crater per metre in a 237.78 square kilometre area. For 38,000 craters per 1 million square km, multiply each by one million. To find 4.0 billion years, and locate 3.8 under 10 to the 4th trace across to the green dotted line 5. Your age estimate for Hadriaca Patera is based on the density of craters equal to or larger than 500 meters in size. Why did we select that size limit for this image? We asked you to focus on 500+ meter craters because

there are enough of them present in a field of this size and this age to give a statistically useful answer. How would your age estimate change if you studied craters down to a limit of 250 meters? Calculate a second age estimate based on these craters, and compare it to your first value. Do they agree? If we use craters at 250 meters we would see it be older. 6. Pavonis Mons Mark all craters equal to or larger than 63 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I discovered 7 craters with a diameter of 63 meters or greater. Because there are so few craters, I estimate the age to be 100,000 years 0.72373114x 1,000,000= 723,731 from solid blue line 3.11x 3.11=9.6721 7(craters)/9.6721= 0.72373114x 1,000,000= 723,731 7. Arsia Mons Mark all craters equal to or larger than 63 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. The age for this surface is 70,000,000 years from the solid line. There are 30 craters that are equal to or larger than 63 meters in diameter 4.36 x 4.36= 19.0096 Number of crater that are greater than 63 meter/19.0096= 1.578x1,000,00=1,578,100 8. Olympus Mons Mark all craters equal to or larger than 16 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work.

I found 3 craters equal or larger to 16 meters 1.60x 1.60= 2.56 3/2.56=1.171875x 1,000,000=1,171,875 Answer is 2,900,000 roughly from Black solid line 9. Which crater field was the most difficult for you to mark, and which was the most straightforward? Is there a connection between the terrain of the surface being sampled and the accuracy with which craters are identified? Does it matter how small the minimum target crater size is, or how well- resolved the image is (the size of the smallest physical structure which can be observed on it)? Olympus Mons was most difficult to see because the craters were not easy to see, or had very few to see. Arsia Mons was most straight forward, many craters could be seen there. The surface being sampled shows enough to provide the information. At the same time there could be more to the actual spot and not just the sampled area. That was a difference. Yes there is a connection between the terrain of the surface being sampled and the accuracy with which craters are identified. The age of a particular surface is proportional to the surface density of crater it has collected. Because larger impact craters are created by larger impactors. Also the image resolution in the study of the crater depends on the minimum target crater size. Because from that the area covered by lava flow, diameter of the crater and every parameters depend upon it. 10. Consider the information given in the text, and Figures 4.3 and 4.4, and explore whether your age estimates for all four volcanic regions agree or disagree with the time line established for the three major epochs of Martian surface evolution. My estimates agree with the time line established Dating Valley Networks and Outflow Channels 1. Nirgal Vallis

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Mark all craters equal to or larger than 500 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I found 12 craters equal to or larger than 500 meters in diameter. 17.39x17.39=302.41 12/302.41= 0.0397x1,000,000= 39,700 2x 10⁹=2,000,000,000 years old from the dotted pink line 2. A crater is observed to cut through the Nirgal Vallis in the view of the surrounding area, suggesting that this water-carved valley is ( older ) than the crater. (Remove incorrect answers.) 3. Tiu Vallis Mark all craters equal to or larger than 250 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I found 27 Craters equal to or greater than 250 meters in diameter. 16.26x16.26=264.3876 27/264.3876=10.212x1,000,000=10,212,000 1.2x10⁹=1,200,000,000 years old roughly from Orange solid line 4. Warrego Vallis Mark all craters equal to or larger than 500 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I found 9 craters equal to or larger than 500 meters in diameter 15.47x15.47=239.3209 9/239.3209=0.0376 x 1,000,000=37,600 4.2x10⁹= 4,200,000,000 years old roughly from pink dotted line 5. Ares Vallis

(a) Mark all craters equal to or larger than 250 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I found 11 craters equal to or larger than 250 meters in diameter 8.20x 8.20=67.24 11/67.24=0.1636x 1,000,000=163,600 1.8x 10⁹=1,800,000,000 years old roughly (b) Water flowed into this region from the ( lower ) - ( right ) corner, and exited via the ( upper ) - ( left ) corner. (Remove incorrect answers.) 6. Based on your estimates of the ages for these four water-carved surfaces, ( outflow channels ) are older. Explain your answer. (Remove incorrect answers.) Dating Water Floods Caused by Volcanic Activity 1. Dao Vallis Mark all craters equal to or larger than 250 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I found 11 craters equal to or larger than 250 meters in diameter 11.64x 11.64=135.4896 11/135.4896=0.0812x 1,000,000=81,200 7x 10⁸=700,000,000 years old roughly 2. Cerberus Fossae Mark all craters equal to or larger than 16 meters in diameter , and then use your measurement of the crater surface density to derive an age for this surface. Show your work. I found 1 crater equal to or larger than 16 meters in diameter

1.53x 1.53=2.3409 1/2.3409=0.4272x 1,000,000=427,200 9x 10⁵= 900,000 years old roughly 3. How do the ages of these two outflow channels compare to those studied in Section 4.5.1? The ages of these two outflow channels seem to be younger in years when compared to the others Final (post-lab) Questions 1. Figure 4.8 contains images of four Jovian moons, all with thin atmospheres. Examine the images and then answer the following questions based on your observations. (a) Sort the four surfaces from oldest to youngest. Why did you rank them in this order? Based off their surfaces I ranked Callisto, Europa, Ganymede, lo from oldest to youngest b) Which moon(s) are most likely to be geologically active, and why? Europa, Ganymede, and lo because of their temperature and pull toward each other 2. Create two histograms, each one counting the total number of craters in a single hemisphere. Do the two histograms support, contradict, or in no way relate to the hypothesis? Explain your reasoning. Make sure to label the axes of both plots, and to include appropriate figure captions. I believe the two histograms “in no way relate to the hypothesis”. I think its

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too hard to get a clear idea using the number of and diameter of craters. A line plot would give us a better idea

3. Could you distinguish between a billion-year old surface and a 3.5 billion- year old surface by counting the surface density of craters with diameters equal to or greater than 16 meters? If so, how? If not, why, and what simple change could you make to your approach to do so? What results (specific values for your measurements) would you expect for each surface? No, you would not be able to distinguish between the two, you would need a different kind of plot. Large craters are easier to use than small ones but the larger ones are more rare as well. A one billion year old surface should have 17,000 times more 125+ meter impact craters than one million year old surface. 4. Figure 4.9 shows a portion of the caldera at the summit of Ceraunius Tholus. You could derive an age for the surface by assuming that all of the craters were caused by impactors. If you then realized that half of them were interlopers (volcanic or collapse features), how would your answer change - would your derived age increase or decrease, and by how much? Explain your answer.

The age would decrease by thousands of years, because craters are typically older when more collisions occur. 5. (a) Describe a possible systematic bias which might affect the measurements of impact crater densities that you made in this laboratory exercise. Using a different apparatus or tool for measurement. (b) If you find four 63+ meter craters in a ten square kilometer field, what age would you derive for the area? If you found two in the adjacent ten square kilometers, what age would you derive from that field? What is the difference between your two estimates, in years? 4,000,000 2,000,000 2,000,000 year difference between the two If you then expanded your field size and found 4,000 63+ meter craters in a ten-thousand square kilometer field and 3,937 in a neighboring field of the same size, what ages would you now derive, and what would the difference be, in years? 40,000,000 and 40,000,000 There would be no difference, it would be the same What can you conclude about the importance of field size in determining surface ages? You need to have a range of measurements for the craters, if not then your calculations could be incorrect. 6. Which of these two models (gradual, or catastrophic processes) best explains the formation of Martian valley networks, and which best explains the formation of Martian outflow channels? Gradual model best explains the formation of martian valley networks and

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martian outflow channels. Summary (300 to 500 words) Mars surface is dry, and covered with old volcanoes and impact craters. The planet is said to be covered by an iron dust, with the consistency of baby powder. The surface is riddled with craters and some of those craters are intact because the environment does not erode them. According to data, the last eruptions occurred on Mars around 25 million years ago. The most recent volcano took place in Olympic mons, and I believe this because astronomers have found volcanic vents in that area. There is also some speculation that mars may still be volcanically active. Water last flowed freely around 2 billion years ago on mars. Many of the studies to estimate this god back to findings of salt deposits on mars. Residue from salt that is believed to from previous water. There is also another theory that mars has water trapped in ice caps frozen, and some experts estimate as much as 100 feet could be there frozen. I do think mars had free flowing water before and there is evidence in minerals. That is also, why I believe the climate has something to do with it because water is trapped in ice caps and within minerals. Studying the geological process on mars can increase our understanding on earth because the two planets share some similarities. Mars has atmosphere, winds, clouds, weather, ice, snowcaps, and dust storms like Earth does. Studying the climate change on Mars can help us understand earth changes. What processes have led to the changes in the planets climate change and what can change will help us better understand earth’s climate. The minerals from hot springs and residue are similar to the hot springs found in Yellowstone Park on earth. So studying how those might have dried up on mars may help us understand those of earth. Studying the magnetic fields on mars also help us solve questions of those on earth. Since mars is so similar to Earth and has gone geological changes, studying those changes will be crucial for helping earth. Extra Credit

While both Barringer and Sunset carter happened in Arizona at different times both are two different types of craters. The barringer crater is a meteorite that is about 50,000 year old. Sunset Crater is crater that was formed by a volcanic eruption. Barriner crater is an impact crater with the diameter of 1.186 km and 560 feet deep. Sunset crater has a diameter of 1.6km wide and about 300 feet deep. Just for reference, most of the diameters of the craters on Mars are 290 km wide and larger. They also do not erode as much as the craters on earth because of the environment.

lab 4 report filled out Astronomy

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