Foundations of Astronomy
13th Edition
ISBN: 9781305079151
Author: Michael A. Seeds, Dana Backman
Publisher: Cengage Learning
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Chapter 20, Problem 3DQ
To determine
The things that can be expected in the surface of a planet on another planetary system when there is oxygen in its atmosphere.
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A new Terrestrial planet has been discovered orbiting a
nearby Sun-like star. Astronomers have obtained spectra
of this planet and determined that the atmosphere is
composed of roughly 99% CO2, and the remaining 1% is
mostly N2 and is very thin compared to Earth's
atmosphere. Briefly describe how the planet could have
developed such an atmosphere.
Chapter 20 Solutions
Foundations of Astronomy
Ch. 20 - Why would you include the Moon in a comparison of...Ch. 20 - Prob. 2RQCh. 20 - Which is the most geologically active Terrestrial...Ch. 20 - In what ways is Earth unique among the Terrestrial...Ch. 20 - Which Terrestrial worlds have thin or no...Ch. 20 - Describe the four stages of Terrestrial planet...Ch. 20 - The Moon did not pass through all of the four...Ch. 20 - Earth shows few craters on its surface. What is...Ch. 20 - How do you know that Earth is differentiated?Ch. 20 - What keeps Earths interior warm today?
Ch. 20 - Lava flows today are examples of basin flooding....Ch. 20 - Describe three forms of erosion that cause slow...Ch. 20 - Prob. 13RQCh. 20 - Which type of seismic wave cannot pass through...Ch. 20 - Prob. 15RQCh. 20 - Which of the five Terrestrial worlds have bow...Ch. 20 - How is the root cause of earthquakes in Hawaii...Ch. 20 - What characteristics must Earths core have to...Ch. 20 - Which of the five Terrestrial worlds have plate...Ch. 20 - Prob. 20RQCh. 20 - How do island chains located in the centers of...Ch. 20 - What evidence can you give that the Atlantic Ocean...Ch. 20 - How are the inferred properties of Earths original...Ch. 20 - Prob. 24RQCh. 20 - Prob. 25RQCh. 20 - Life on Earth exists because of oxygen in Earths...Ch. 20 - Prob. 27RQCh. 20 - Prob. 28RQCh. 20 - Prob. 29RQCh. 20 - Prob. 30RQCh. 20 - Prob. 31RQCh. 20 - Prob. 32RQCh. 20 - Why would a decrease in the density of the ozone...Ch. 20 - How Do We Know? How can the flow of energy out of...Ch. 20 - Prob. 35RQCh. 20 - Prob. 1DQCh. 20 - Prob. 2DQCh. 20 - Prob. 3DQCh. 20 - Prob. 4DQCh. 20 - Prob. 5DQCh. 20 - Prob. 6DQCh. 20 - Look at Figure 19-3. The earthquake occurred 7440...Ch. 20 - Look at Figure 19-3. The lag time is the...Ch. 20 - What percentage of Earths volume is the metallic...Ch. 20 - How many magnetic pole reversals has Earth endured...Ch. 20 - If the Atlantic seafloor is spreading at 3.0...Ch. 20 - The Hawaiian-Emperor chain of undersea volcanoes...Ch. 20 - From Hawaii to the bend in the Hawaiian-Emperor...Ch. 20 - Prob. 9PCh. 20 - Prob. 1LTLCh. 20 - Look at the hemispheres of Earth shown on the two...Ch. 20 - Prob. 3LTLCh. 20 - Look at Figure 19-9. Rising from Earths surface to...Ch. 20 - Prob. 5LTLCh. 20 - What do you see in this photo that suggests heat...
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- The fraction of the energy flux received which is reflected into space is the albedo of Venus, av, which is about 0.76. The fraction of the energy flux which is absorbed is then (1-av) = 1. - 0.76 = 0.24. So the amount of energy actually absorbed by Venus in each second is Lv = (1-av)Ev. Lv = (1-av)Ev = ___________________ ergs/s And next calculate the effective temperature of Venus: Tv4 = (Lv/(4pdv2))/s = Lv/(4spdv2) = __________________ K4 and taking the square root of Tv4 twice in succession we get the effective Temperature Tv: Tv = [Lv/(4spdv2)]0.25 = _________________ K Calculate Venus' emittance assuming that the Venus' actual temperature, Tvr, is 472o C = 745 K: ev = Lv/(4pdv2s Tvr4) = __________________ .arrow_forwardCalculate the pressure p of the Venus atmosphere (it consists of CO2 at 477oC) at the height of 1 km from the planet surface, where p0=9.3 MPa. The planet mass is 4.9x1024 kg, its radius is 6050 kmarrow_forwardIf liquid water is rare on the surface of planets, then most Terrestrial planets must have CO₂-rich atmospheres. Why?arrow_forward
- 100% Normal text Arlal 12.5 | I1 1 | 2 | 3 3. Fill out this data table with information you have collected about the solar system planets. Characteristics Unit Mercury Venus Earth 330 4,870 5,970 Mass 1024 g 61 928 1,083 Volume 1024 cm3 5.4 5.4 50 Density g/cm3 58 106 km 100 100 Distance from Sun Radius km Crust Thickness km Atmosphere Height kmarrow_forwardFill 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_forwardLook at Figure 21-11. Which molecule(s) can escape from Earths gravity? From Mars? From Venus? Figure 21-11 Loss of atmospheric gases. Dots represent the escape velocity and temperature of various Solar System bodies. The lines represent the typical highest velocities of molecules of various masses. The Jovian planets have high escape velocities and can hold onto even the lowest-mass molecules. Mars can hold only the more massive molecules, and the Moon has such a low escape velocity that even massive molecules can escape.arrow_forward
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