Inner planets e version(1)

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Inner Solar System Planets Select the Inner Solar System link to complete this lab. A. Select Mercury 1. Using the Go directly to image (PI XXXXX) box, type in PIA02943 . Hit enter View the photo 300 km Long Scarp. Q1. What caused this feature? The 300 km Long Scarp on Mercury was caused by the planet's crust cooling and contracting, leading to the formation of large faults 2. Select Mercury from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA02438 . Hit enter View the photo Heavily Cratered Terrain and Smooth Plain. Q2. These features make Mercury look similar to what other member of the solar system? The heavily cratered terrain and smooth plain on Mercury make the planet look similar to Earth's moon.1 B. Select Venus from the Image Gallery 1. Venus has three main surface features are volcanoes, highlands and rolling plains . Identify these three features in the following two photos. Using the Go directly to image (PI XXXXX) box, type in PIA00093 . Hit enter. View the photo Perspective View Ishta Terra. Q1. What are the red areas shown in this photo? The red areas shown in the photo Perspective View Ishta Terra are likely to be areas of higher elevation, possibly mountainous or highland regions. The red color is indicative of this higher elevation. 2. Select Venus from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00159 . Hit enter View photo Hemisphere View of Venus Centered 180 degrees. Q2. What is the large red/pink region? The large red/pink region in the photo

Hemisphere View of Venus Centered 180 degrees is known as Alpha Regio. It is a highland region on Venus that rises about 2-3 kilometers above the surrounding plains. Q3. What is the blue/green area? The blue/green area in the photo Hemisphere View of Venus Centered 180 degrees is called Atla Regio. It is also a highland region on Venus, but it is smaller and less elevated than Alpha Regio. 3. Select Venus from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00103 . Hit enter View photo Venus 3D Perspective View of Lavinia Planitia. Q4. What is the large central object? The large central object in the photo Venus 3D Perspective View of Lavinia Planitia is likely a volcanic feature called a shield volcano. It appears relatively flat and is surrounded by a circular depression, which is a common feature of shield volcanoes. 4. Select Venus from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00102 . Hit enter View photo Venus 3D Perspective View of Estla Regio. Q5. What is the elevated object in the top left of the photo? B5. The elevated object in the top left of the photo Venus 3D Perspective View of Estla Regio is likely a volcanic feature called a coronae. Coroanae are circular to elliptical-shaped structures, often surrounded by a raised ridge, and are thought to be caused by upwelling material from the interior of the planet resulting in deformation of the surface. 5. Select Venus from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00268 . Hit enter

View photo Venus 3D Perspective of Latona Corona & Dali Chasma Q6. What mineral is found on the scrap? Basaltic rocks 6. Select Venus from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00246 . Hit enter View photo Venus 3D View of Eastern Edge of Alpha Regio. Q7. What is the cause of these “hills”? The cause of the "hills" seen in the photo Venus 3D View of Eastern Edge of Alpha Regio (PIA00246) is not explicitly mentioned in the photo or its caption. However, it is possible that they are the result of tectonic or volcanic activity, which can cause deformation and uplift of the crust. The highlands in the Alpha Regio region are known to be the result of volcanic activity, so it is possible that the hills seen in the photo are also related to this volcanic activity. 7. Select Venus from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00072 . Hit enter View photo Venus Cloud Patterns (colorized & filtered) Q8. From what are the clouds made? The clouds seen in the photo Venus Cloud Patterns (colorized & filtered) (PIA00072) are mainly composed of sulfuric acid. Venus has a thick atmosphere that is dominated by carbon dioxide, and the clouds are composed of droplets of sulfuric acid that form at an altitude of about 50- 70 km above the surface. The cloud patterns seen in the photo are the result of atmospheric circulation and convection, similar to weather patterns on Earth. C. Select Mars from Image Gallery 1. Using the Go directly to image (PI XXXXX) box, type in PIA01004 . Hit enter View photo ASI / MET within color-enhanced panorama. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00979 . Hit enter View photo Roadrunner Flats Q1. What is the color of the Martian soil? The color of the Martian soil varies depending on the location, but in general, it is reddish-brown in color. In the photo

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Roadrunner Flats (PIA00979), the soil appears to be a rusty-red color, which is a common color for Martian soil due to the presence of iron oxide (rust). In the photo ASI / MET within color-enhanced panorama (PIA01004), the soil also appears to be reddish-brown, with some lighter-colored areas that may indicate the presence of different minerals or materials. 2. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA01466 . Hit enter View photo Improved MPF 360 degree color Panorama. Q2. What features and rocks are seen in this photo? The photo Improved MPF 360 degree color Panorama (PIA01466) shows a wide range of features and rocks on the surface of Mars. Some of the features include: - Mountains and hills: There are several mountains and hills visible in the distance, including the large central peak of Gale Crater, which is the focus of the Curiosity rover's mission. - Crater rims and floors: There are numerous craters visible in the photo, both in the foreground and in the distance. Some of these craters have visible rims and floors that can be examined in detail. - Rock formations: There are many interesting rock formations visible in the photo, including layered sedimentary rocks that were deposited by ancient water or wind, and small, rounded rocks that may have been shaped by erosion. - Sand dunes: There are several large sand dunes visible in the foreground of the photo. These dunes are made up of dark, basaltic sand that has been blown into various shapes by the wind. - Rover tracks: In some areas of the photo, you can see the tracks left by the Curiosity rover as it explores the Martian landscape.

3. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00407 . Hit enter View photo Global Color View of Mars. Q3. What is the top feature? In the photo Global Color View of Mars (PIA00407), it is difficult to determine one top feature as the photo shows the entire planet Mars. However, some prominent features that can be seen in the photo include the dark, low-lying plains in the northern hemisphere (known as the "Viking Northern Plains"), and the large, circular depression in the southern hemisphere (known as the Hellas Basin). Q4. What is the feature in the center just below the equator? The feature in the center just below the equator in the Global Color View of Mars (PIA00407) appears to be the Tharsis volcanic plateau. This is a large volcanic plateau located near the equator on the western side of Mars, and it contains several large shield volcanoes, including Olympus Mons, which is the largest volcano in the solar system. 4. Select Mars from the Image Gallery. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00006 . Hit enter View photo Oblique View with Altimetry of Valles Marineris. Q5. What formed this feature? The Valles Marineris on Mars was formed by a combination of tectonic forces and erosion. It is believed that the initial formation of the canyon was due to tectonic stretching and cracking of the Martian crust, possibly caused by the planet's interior cooling and contracting. Subsequent erosion from wind, water (in its past), and other geological processes then widened and deepened the canyon over time. 5. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA02844 . Hit enter View the photo Sediment History Persevered in Gale Crater. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA02824 . Hit enter View the photo Channeled Aprons Q6. These photos show evidence of what flowed on Mars? Both the photos - "Sediment History Preserved in Gale Crater" (PIA02844) and "Channeled Aprons" (PIA02824) - show evidence of water flowing on Mars. In the first photo, the layers of sedimentary rock in Gale Crater suggest that water was once present in a large lake in the area, and the various layers built up over time as sediment settled to the bottom. In the second photo, the channeled aprons suggest that glaciers or water flows carved out channels into the surrounding hillsides, leaving sediment and

debris at the base of the slopes. These features indicate that water was once flowing on the surface of Mars. 6. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA02806 . Hit enter View photos Major Martian Volcanoes from MOLA Q7. What is this? The photo "Major Martian Volcanoes from MOLA" (PIA02806) shows a topographic map - specifically, an elevation model - of the Martian surface. It highlights the major volcanoes on Mars, including Olympus Mons, which is the largest known volcano in the Solar System. It was created using data from the Mars Orbiter Laser Altimeter (MOLA), which measured the elevation of features on the Martian surface using pulsed laser beams. 7. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA01476 . Hit enter View the photo Olympus Mons. Q8. How tall and wide is it? The photo "Olympus Mons" (PIA01476) shows an oblique view of the largest known volcano in the Solar System, which is located on the surface of Mars. Olympus Mons is a shield volcano that measures approximately 22 km (14 miles) high and 550 km (342 miles) wide at its base. Its summit caldera is over 80 km (50 miles) wide, and contains multiple smaller volcanic vents. The volcano's sheer size is due to the fact that Mars lacks plate tectonics, so the volcano has been able to continue erupting in the same spot for billions of years, building up its massive size. 8. Select Mars from the Image Gallery. Using the Go directly to image (PI XXXXX) box, type in PIA00784 . Hit enter View the photo Clouds over Mars. Q9. What are the clouds composed of? The photo "Clouds over Mars" (PIA00784) shows a view of an extensive cloud system over the Martian south pole, as seen by NASA's Viking Orbiter 1 spacecraft in 1978. The clouds are composed of water ice crystals, which are thought to form at high altitudes in the Martian atmosphere where temperatures are cold enough for water to freeze. These clouds play an important role in the Martian climate by reflecting sunlight back into space, which helps to cool the planet. They also contribute to the Martian water cycle by releasing precipitation in the form of snow or frost onto the polar regions. 4 9. Using the Go directly to image (PI XXXXX) box, type in PIA00915 . Hit enter

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View the photo Violet Martian Sky Q10. What size are the particles? The photo "Violet Martian Sky" (PIA00915) shows a view of the hazy atmosphere above the surface of Mars, captured by NASA's Viking Orbiter 1 spacecraft in 1976. The bluish-violet color of the sky is due to the presence of fine dust particles in the atmosphere, which scatter sunlight in a way that is similar to the effect that makes the sky appear blue on Earth. According to NASA, the dust particles that give Mars its hazy appearance are typically estimated to be around 1 micron in size, which is about one-thousandth the diameter of a human hair. 10. Using the Go directly to image (PI XXXXX) box, type in PIA01334 . Hit enter View the photo High- Resolution MOC Image of Phobes Q11. What is the name of the largest crater on Phobes? The photo "High- Resolution MOC Image of Phobos" (PIA01334) shows an oblique view of Phobos, the larger of the two moons of Mars, taken by NASA's Mars Global Surveyor spacecraft in 1998. There are several craters visible on the surface of Phobos in this image, but the largest one is called Stickney crater. Q12. What is the size of this crater? Stickney crater on Phobos is approximately 9 kilometers (5.6 miles) in diameter, which is about one-third the diameter of the moon itself. The crater is so large that it almost completely dominates one end of Phobos, and its impact is believed to have created the grooves and linear features visible on the moon's surface. D. Select Small Bodies from the Image Gallery 1. Using the Go directly to image (PI XXXXX) box, type in PIA00333 . Hit enter View the photo Asteroid Ida and its satellite. Q1. From what material is this asteroid made? The photo "Asteroid Ida and its satellite" (PIA00333) shows the asteroid 243 Ida and its small natural satellite Dactyl. Ida is a rocky S-type asteroid, which means it is made primarily of silicate minerals, such as pyroxene and olivine, as well as metal-rich minerals like iron and nickel. The composition of Ida is similar to that of many meteorites that have been found on Earth, which suggests that S-type asteroids like Ida may be the parent bodies of some types of meteorites.

2. Select Small Bodies from the Image Gallery Using the Go directly to image (PI XXXXX) box, type in PIA03109 . Hit enter View photo Hint of Structure. Q2. What caused the odd features? The photo "Hint of Structure" (PIA03109) shows the asteroid Eros, which was imaged by NASA's NEAR Shoemaker spacecraft in 2001. The odd features visible on Eros were caused by a combination of factors, including impact events, internal stresses caused by the asteroid's rotation and changing temperature, and the movement of material downslope due to gravity. For example, some of the linear features on Eros may be fractures or faults that formed when the asteroid was jolted by a nearby impact, while other features, such as the smooth areas and the rounded mounds, may have been shaped by landslides or other movement of material downslope. 3. Using the Go directly to image (PI XXXXX) box, type in PIA15678 . Hit enter View photo Full view of Vesta. Q3. How tall is the mountain at the south pole? The photo "Full view of Vesta" (PIA15678) shows the asteroid Vesta, which was imaged by NASA's Dawn spacecraft in 2011-2012. The tall mountain at Vesta's south pole is called Rheasilvia, and it is approximately 22 km (14 miles) high. This makes Rheasilvia one of the tallest mountains in the solar system, and it is thought to be the result of a large impact that excavated a basin on Vesta's surface and created a central peak. 5

Inner planets e version(1)

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