Astronomy
1st Edition
ISBN: 9781938168284
Author: Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher: OpenStax
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Textbook Question
Chapter 12, Problem 20E
We have a lot of good images of the large moons of Jupiter and Saturn from the Galileo and Cassini spacecraft missions (check out NASA’s Planetary Photojournal site, at http://photojournal.jpl.nasa.gov, to see the variety). Now that the New Horizons mission has gone to Pluto, why don’t we have as many good images of all sides of Pluto and Charon?
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The ratio of charon to pluto's roche limit? or
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In 2015, researchers concluded that Enceladus's subsurface ocean is probably global, instead of just being restricted to the south polar region. What had the Cassini spacecraft found, that led them to their conclusion?
a Enceladus wobbles slightly as it orbits Saturn, more so than it could if its ice shell were mostly frozen to the rocky interior.
b Enceladus is absorbing so much water (which is ejected by Saturn from its atmosphere) that there must be a global ocean under its icy surface.
c The number of large, lava-spewing volcanoes on Enceladus's surface is so high that they can only be the result of liquid water under the whole surface.
d The magnetic field of Enceladus is so strong that it can only be explained by a global ocean of salty water under the surface.
Assuming all other variables were earth based besides atmospheric pressure, calculate the temperature at which water would boil at sea level on Titan versus Earth? And explain why using molecular concepts. Consider the pressure of Earth’s atmosphere at sea level to be 1 atm and the pressure of Titan’s atmosphere at sea level to be 1.45 atm.
ps plz stop refusing my questions or im going to cancel this membership
Chapter 12 Solutions
Astronomy
Ch. 12 - What are the moons of the outer planets made of,...Ch. 12 - Compare the geology of Callisto, Ganymede, and...Ch. 12 - What is the evidence for a liquid water ocean on...Ch. 12 - Explain the energy source that powers the...Ch. 12 - Compare the properties of Titan’s atmosphere with...Ch. 12 - How was Pluto discovered? Why did it take so long...Ch. 12 - How are Triton and Pluto similar?Ch. 12 - Describe and compare the rings of Saturn and...Ch. 12 - Why were the rings of Uranus not observed directly...Ch. 12 - List at least three major differences between...
Ch. 12 - The Hubble Space Telescope images of Pluto in 2002...Ch. 12 - Saturn’s E ring is broad and thin, and far from...Ch. 12 - Why do you think the outer planets have such...Ch. 12 - Ganymede and Callisto were the first icy objects...Ch. 12 - Compare the properties of the volcanoes on Io with...Ch. 12 - Would you expect to find more impact craters on Io...Ch. 12 - Why is it unlikely that humans will be traveling...Ch. 12 - Why do you suppose the rings of Saturn are made of...Ch. 12 - Suppose you miraculously removed all of Saturn’s...Ch. 12 - We have a lot of good images of the large moons of...Ch. 12 - In the Star Wars movie Star Wars Episode VI:...Ch. 12 - Which would have the longer orbital period: a moon...Ch. 12 - How close to Uranus would a spacecraft have to get...Ch. 12 - Saturn’s A, B, and C Rings extend 75,000 to...Ch. 12 - Use the information in Appendix G to calculate...Ch. 12 - The average distance of Enceladus from Saturn is...
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Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- We believe that chains of comet fragments like Comet Shoemaker-Levy 9’s have collided not only with the jovian planets, but occasionally with their moons. What sort of features would you look for on the outer planet moons to find evidence of such collisions? (As an extra bonus, can you find any images of such features on a moon like Callisto? You can use an online site of planetary images, such as the Planetary Photojournal, at photojournal.jpl.nasa.gov.)arrow_forwardPresent theory suggests that giant planets cannot form without condensation of water ice, which becomes vapor at the high temperatures close to a star. So how can we explain the presence of jovian-sized exoplanets closer to their star than Mercury is to our Sun?arrow_forwardCompare the interior cutaway sketches of the four Jovian planets in their Celestial Profiles. What interior layer(s) is (are) shown in Jupiter and Saturn but not in Uranus and Neptune, and vice versa?arrow_forward
- Upload a PDF document that shows your work and solution. - Consider a moon of Uranus if Uranus is currently a distance of 2.08 billion km from Earth, then what diameter telescope would you need (use telescope-resolution formula = 1.22, where D is the telescope diameter) in order to clearly resolve the moon Titania in orbit around Uranus if the 47² )3 to relate moon has a period of orbit of T = 8.71 days? (use Kepler's 3rd Law T² = (GMrave T2 moon's period T to moon's orbital radius, r) The telescope only needs to resolve the small dot of the moon as distinct from the circle of light which is Uranus, so the orbital resolution is the angular size of the diameter of orbit of Miranda (use the arc-length formula 0 = 2 where d is the distance from Earth to Uranus). Take the mass of Uranus as 8.68 × 1025 kg, and the wavelength of light as 490 d nm.arrow_forwardIf Earth-based telescopes can resolve angles down to 0.25 arcsec, how large could a trans-Neptunian object be at Pluto’s average distance from the Sun and still not present a resolvable disk?arrow_forwardCalculate the radius of Jupiters Roche limit for a satellite with density equal to the planet. Which of Jupiters moons is closest to the Roche limit? What might that tell you about the relationship between that moon and Jupiters ring? (Note: Necessary data are given in Celestial Profile: Jupiter and Appendix Table A-11.)arrow_forward
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