Loose Leaf For Explorations: Introduction To Astronomy
9th Edition
ISBN: 9781260432145
Author: Thomas T Arny, Stephen E Schneider Professor
Publisher: McGraw-Hill Education
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Chapter 10, Problem 3TY
To determine
Correct statement about the Roche limit.
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You are making a scale model to visualize the relative sizes of the planets in our solar system. The scale of the model is: 1 cm = 2000 km. The radius of Saturn is 60,000 km. At what radius will Saturn appear on your scale model?
What is the range of density for the outer planets (in g/cm3)?
1.2 to 5.5
2.2 to 5.5
2.2 to 6.5
3.3 to 7.2
none of these
i legacynv.schoology.com/common-assessment-dlelivery/start/48958977
Kuiper Belt
Jupiter
Mercury
Venus
Urahus
Saturn
Mars
Farth
· Ceres
Neptune
Jupiter
Pluto
inner solar system
outer solar system
not to scale
Is this model to scale regarding the sizes of the planets and distances between them? Why or why not?
O Yes. That is why the outer planets are shown in a separate box.
O No. The distances in the solar system are too great to produce a model accurate to distance that still has inner planets visible.
O No. The outer planet distances are drawn to scale, but the inner planets need to be drawn farther from the sun to be visible.
1
4
Chapter 10 Solutions
Loose Leaf For Explorations: Introduction To Astronomy
Ch. 10 - Prob. 1QFRCh. 10 - What does Jupiter look like?Ch. 10 - How do astronomers know what lies inside the outer...Ch. 10 - What are the major gaseous substances that make up...Ch. 10 - What is the interior structure of Jupiter and...Ch. 10 - Do Jupiter and Saturn have solid surfaces?Ch. 10 - Prob. 7QFRCh. 10 - Prob. 8QFRCh. 10 - What sort of activity has been seen on Io? What is...Ch. 10 - What are the rings of Saturn made of? How do...
Ch. 10 - Prob. 11QFRCh. 10 - Prob. 12QFRCh. 10 - Prob. 13QFRCh. 10 - What is unusual about Uranuss rotation axis? What...Ch. 10 - Prob. 15QFRCh. 10 - Why are Uranus and Neptune so blue?Ch. 10 - Why are the outer planets so large?Ch. 10 - Prob. 18QFRCh. 10 - Prob. 1TQCh. 10 - Prob. 2TQCh. 10 - Ganymede and Callisto orbiting Jupiter and Tethys...Ch. 10 - Approximate the Roche limit as 2.44 times a...Ch. 10 - Prob. 5TQCh. 10 - (10.3) Is Uranuss sky blue for the same reason our...Ch. 10 - Prob. 7TQCh. 10 - Prob. 8TQCh. 10 - Prob. 9TQCh. 10 - Prob. 10TQCh. 10 - Prob. 1PCh. 10 - Prob. 2PCh. 10 - Prob. 3PCh. 10 - Prob. 4PCh. 10 - Prob. 5PCh. 10 - Prob. 6PCh. 10 - Prob. 7PCh. 10 - Prob. 8PCh. 10 - (10.1) The low average densities of Jupiter and...Ch. 10 - Prob. 2TYCh. 10 - Prob. 3TYCh. 10 - Prob. 4TYCh. 10 - Prob. 5TYCh. 10 - Prob. 6TYCh. 10 - Prob. 7TY
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- You are a planetary scientist studying the atmosphere of Jupiter through a large telescope when you observe an asteroid approaching the planet. This asteroid is large, so you know it is held together by gravity rather than the cohesive forces that hold a large rock together. If the asteroid gets too close to Jupiter, the massive tidal forces will tear it apart, scattering small particles that will add to the ring system. You have calculated the closest distance the asteroid will come to Jupiter. How do you know if the asteroid will survive? a. A measure of the cohesive gravitational force holding such an asteroid together is the gravitational field on the surface due to the mass of the asteroid. This field is independent of the distance of the asteroid from Jupiter. Calculate the gravitational field at the surface of the asteroid due only to the mass of the asteroid. Assume the asteroid has a diameter of 10,000 km and a density of 1300 kg/m3. b. Tidal forces from Jupiter tend to disrupt the asteroid by pulling it apart. The tidal forces depend on the distance between Jupiter and the asteroid. There is a distance between Jupiter and the asteroid known as the Roche limit where the tidal forces are balanced by the asteroids own cohesive gravitational force. If the asteroid is within the Roche limit, it will be torn apart. Figure P7.60 shows Jupiters gravitational field as a function of distance from its center. By looking at this graph, can you determine an approximate value for the Roche limit for this asteroid in the vicinity of this planet? c. What will happen to the Roche limit if we consider an asteroid of lower density? FIGURE P7.60arrow_forwardLook at Appendix F and Appendix G and indicate the moon with a diameter that is the largest fraction of the diameter of the planet or dwarf planet it orbits.arrow_forwardV5arrow_forward
- Fill out this data table with information you have collected about the solar system planets. Characteristics Unit Mercury Venus Earth 330 10 g 4,870 5,970 Mass 61 928 1,083 Volume 1024 cm 5.4 5.4 50 Density g/cm Distance from Sun 58 10° km 100 100 Radius km Crust Thickness km Atmosphere Height km Axial Tilt degrees Force of Gravity on a1 kg test mass N Length of Day 4223 4,223 88 hours 225 365 Length of Orbit Earth days 88 167 464 15 Mean Temperature ° C ТЕВОС Mars Jupiter Saturn Uranus Neptune 102,000 642 | 1,898,000 568.000 86,800arrow_forward20 Approximately how many other planetary systems have been discovered to date? A Tens of thousands B) Tens C Hundreds D Thousands E Millionsarrow_forwardMiller’s Planet part I: This planet is described as having 130% Earth gravity What is the acceleration due to gravity on the surface of this planet? 7 m/s2 130 m/s2 13 m/s2 Miller’s Planet part II: What is the source of the waves on this planet? Wind Tidal stress due to proximity of Gargantua Plate tectonic driven Miller-quakes Miller’s Planet Part III: Why would it be unlikely that this planet could sustain an atmosphere let alone liquid water on its surface. Gargantua’s accretion disk likely emits X-rays, UV rays and possibly gamma radiation Miller’s planet’s surface gravity is too small Miller’s planet has no magnetic fieldarrow_forward
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