Nuclear fusion takes place Corona Heat is transferred by "warm air rise, cold air sink" Convection zone principle Heat is transferred by photons of light and it takes the longest time for energy moving outward Radiation zone This layer defines the surface of the Sun Photosphere The outermost layer Core

Nuclear fusion takes place Corona Heat is transferred by "warm air rise, cold air sink" Convection zone principle Heat is transferred by photons of light and it takes the longest time for energy moving outward Radiation zone This layer defines the surface of the Sun Photosphere The outermost layer Core

Stars and Galaxies

9th Edition

ISBN:9781305120785

Author:Michael A. Seeds, Dana Backman

Publisher:Michael A. Seeds, Dana Backman

Chapter8: The Sun

Section: Chapter Questions

Problem 7P

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Similar questions

Why are measurements of the Sun's 10.7 cm radio emission used to monitor the state of the solar cycle? Choose allcorrect answers.A. It provides a repeatable, objective measurement of solar activityB. It serves as a good proxy for EUV emissionsC. It is measured from space, so it is not affected by cloudsD. It can be used to predict the occurrence of coronal mass ejections
How does activity on the Sun affect human technology on Earth and in the rest of the solar system?
Make a sketch of the Sun’s atmosphere showing the locations of the photosphere, chromosphere, and corona. What is the approximate temperature of each of these regions?
Starting from the core of the Sun and going outward, the temperature decreases. Yet, above the photosphere, the temperature increases. How can this be?
What it the Zeeman effect and what does it tell us about the Sun?
Suppose you live in northern Canada and an extremely strong flare is reported on the Sun. What precautions might you take? What might be a positive result?
Add 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.
This chapter gives the average sunspot cycle as 11 years. Verify this using Figure 15.26. Figure 15.26 Numbers of Sunspots over Time. This diagram shows how the number of sunspots has changed with time since counts of the numbers of spots began to be recorded on a consistent scale. Note the low number of spots during the early years of the nineteenth century, the Little Maunder Minimum. (credit: modification of work by NASA/ARC)
Suppose an (extremely hypothetical) elongated sunspot forms that extends from a latitude of 30° to a latitude of 40° along a fixed of longitude on the Sun. How will the appearance of that sunspot change as the Sun rotates? (Figure 15.17 should help you figure this out.) Figure 15.17 Magnetic Field Lines Wind Up. Because the Sun spins faster at the equator than near the poles, the magnetic fields in the Sun tend to wind up as shown, and after a while make loops. This is an idealized diagram; the real situation is much more complex.
What do measurements of the number of neutrinos emitted by the Sun tell us about conditions deep in the solar interior?
If a sunspot has a temperature of 4200 K and the average solar photosphere has a temperature of 5780 K, how much 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, Eq. 7-1.)
From 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))