Essential Cosmic Perspective
9th Edition
ISBN: 9780135795033
Author: Bennett
Publisher: PEARSON
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Chapter 11, Problem 48EAP
To determine
The possibility of human activity affecting the sun.
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If a sunspot has a temperature of 4,270 K and the average solar photosphere has a temperature of 5,780 K, how many times more energy is emitted in 1 second from a square meter of the photosphere compared to a square meter of the sunspot? (Hint: Use the Stefan-Boltzmann law,
E = σT4 (J/s/m2)
where E is the energy, σ is a proportionality constant equal to 5.67 ✕ 10−8 J/s/m2/K4, and T is the temperature in kelvins.)
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Chapter 11 Solutions
Essential Cosmic Perspective
Ch. 11 - Prob. 1VSCCh. 11 - Prob. 2VSCCh. 11 - Prob. 3VSCCh. 11 - Prob. 1EAPCh. 11 - Prob. 2EAPCh. 11 - Prob. 3EAPCh. 11 - Prob. 4EAPCh. 11 - Prob. 5EAPCh. 11 - Prob. 6EAPCh. 11 - Prob. 7EAP
Ch. 11 - Prob. 8EAPCh. 11 - Prob. 9EAPCh. 11 - Prob. 10EAPCh. 11 - Prob. 11EAPCh. 11 - Prob. 12EAPCh. 11 - Prob. 13EAPCh. 11 - Prob. 14EAPCh. 11 - Prob. 15EAPCh. 11 - Prob. 16EAPCh. 11 - Prob. 17EAPCh. 11 - Prob. 18EAPCh. 11 - Prob. 19EAPCh. 11 - Prob. 20EAPCh. 11 - Prob. 21EAPCh. 11 - Prob. 22EAPCh. 11 - Prob. 23EAPCh. 11 - Prob. 24EAPCh. 11 - Prob. 25EAPCh. 11 - Which of these groups of particles has the...Ch. 11 - Prob. 27EAPCh. 11 - Prob. 28EAPCh. 11 - Prob. 29EAPCh. 11 - Prob. 30EAPCh. 11 - Prob. 31EAPCh. 11 - Prob. 32EAPCh. 11 - Prob. 33EAPCh. 11 - 34. What causes the cycle of solar activity? (a)...Ch. 11 - 35. Which of these things poses the greatest...Ch. 11 - Prob. 37EAPCh. 11 - Prob. 38EAPCh. 11 - Prob. 39EAPCh. 11 - Prob. 41EAPCh. 11 - Prob. 42EAPCh. 11 - Prob. 43EAPCh. 11 - Prob. 44EAPCh. 11 - Prob. 45EAPCh. 11 - Prob. 46EAPCh. 11 - Prob. 47EAPCh. 11 - Prob. 48EAPCh. 11 - Research: Current Solar Weather. Daily information...Ch. 11 - Prob. 51EAPCh. 11 - Prob. 52EAPCh. 11 - Prob. 53EAPCh. 11 - Prob. 54EAPCh. 11 - Prob. 55EAPCh. 11 - Prob. 56EAP
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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
- How does activity on the Sun affect human technology on Earth and in the rest of the solar system?arrow_forwardDescribe in your own words what is meant by the statement that the Sun is in hydrostatic equilibrium.arrow_forwardDo you think that nuclear fusion takes place in the atmospheres of stars? Why or why not?arrow_forward
- Explain how mathematical computer models allow us to understand what is going on inside of the Sun.arrow_forwardDescribe how energy makes its way from the nuclear core of the Sun to the atmosphere. Include the name of each layer and how energy moves through the layer.arrow_forwardWhat it the Zeeman effect and what does it tell us about the Sun?arrow_forward
- As we’ve seen, the sun’s energy comes from fusion reactions that combine four hydrogen atoms to produce a single helium atom. Even in the sun’s core, where these reactions proceed most rapidly, the reaction rate is very slow, with only about 6.7 * 1013 reactions per second occurring in 1 cubic meter ofthe core. How much power is produced by these fusion reactions per cubic meter? Compare this number with the 300 W/m3 metabolic power produced by a resting reptile.arrow_forwardWhat are solar cells, how do they work?arrow_forwardFrom the information in Figure 15.21, estimate the speed with which the particles in the CME in parts (c) and (d) are moving away from the Sun. Figure 15.21 Flare and Coronal Mass Ejection. This sequence of four images shows the evolution over time of a giant eruption on the Sun. (a) The event began at the location of a sunspot group, and (b) a flare is seen in far-ultraviolet light. (c) Fourteen hours later, a CME is seen blasting out into space. (d) Three hours later, this CME has expanded to form a giant cloud of particles escaping from the Sun and is beginning the journey out into the solar system. The white circle in (c) and (d) shows the diameter of the solar photosphere. The larger dark area shows where light from the Sun has been blocked out by a specially designed instrument to make it possible to see the faint emission from the corona. (credit a, b, c, d: modification of work by SOHO/EIT, SOHO/LASCO, SOHO/MDI (ESA & NASA))arrow_forward
- The text says that the Local Fluff, which surrounds the Sun, has a temperature of 7500 K and a density 0.1 atom per cm3. The Local Fluff is embedded in hot gas with a temperature of 106 K and a density of about 0.01 atom per cm3. Are they in equilibrium? (Hint: In pressure equilibrium, the two regions must have nT equal, where n is the number of particles per unit volume and T is the temperature.) What is likely to happen to the Local Fluff?arrow_forwardAdd a fourth column to Table 13-1 and write in the atomic mass for each rows fuel element (see Appendix Table A-14). Review the curve of binding energy, Figure 8-15. Explain the trend of fusion time versus fuel atomic mass.arrow_forward
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