21st Century Astronomy
6th Edition
ISBN: 9780393428063
Author: Kay
Publisher: NORTON
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Chapter 14.3, Problem 14.3CYU
To determine
The reason for sharp appearance of sun’s surface in visible light.
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Students have asked these similar questions
The Sun's photosphere is
a. the central region where the Sun originates
b. the part of the Sun which the light comes that we see when we look at the Sun with our eyes
c. the hottest region of the Sun
d. the outermost layers of the Sun's atmosphere
e. the first region you would come to when leaving the core
The capture of too few solar neutrinos by Davis in the solar neutrino experiment
a.
can be explained if the sun is not undergoing thermonuclear fusion of hydrogen in its core.
b.
indicates that the sun’s core is much cooler than expected.
c.
indicates that the sun’s core is much hotter than expected.
d.
indicates that the sun’s core is convective.
e.
is explained by none of the above.
13 What is the solar wind?
(A) The uppermost layer of the Sun, lying just above the corona
B
A stream of charged particles flowing outward from the surface of the Sun
с
D
The wind that causes huge arcs of gas to rise above the Sun's surface
The strong wind that blows sunspots around on the surface of the Sun
Chapter 14 Solutions
21st Century Astronomy
Ch. 14.1 - Prob. 14.1ACYUCh. 14.1 - Prob. 14.1BCYUCh. 14.2 - Prob. 14.2CYUCh. 14.3 - Prob. 14.3CYUCh. 14.4 - Prob. 14.4CYUCh. 14 - Prob. 1QPCh. 14 - Prob. 2QPCh. 14 - Prob. 3QPCh. 14 - Prob. 4QPCh. 14 - Prob. 5QP
Ch. 14 - Prob. 6QPCh. 14 - Prob. 7QPCh. 14 - Prob. 8QPCh. 14 - Prob. 9QPCh. 14 - Prob. 10QPCh. 14 - Prob. 11QPCh. 14 - Prob. 12QPCh. 14 - Prob. 13QPCh. 14 - Prob. 14QPCh. 14 - Prob. 15QPCh. 14 - Prob. 16QPCh. 14 - Prob. 17QPCh. 14 - Prob. 18QPCh. 14 - Prob. 19QPCh. 14 - Prob. 20QPCh. 14 - Prob. 21QPCh. 14 - Prob. 22QPCh. 14 - Prob. 23QPCh. 14 - Prob. 24QPCh. 14 - Prob. 25QPCh. 14 - Prob. 26QPCh. 14 - Prob. 27QPCh. 14 - Prob. 28QPCh. 14 - Prob. 29QPCh. 14 - Prob. 30QPCh. 14 - Prob. 31QPCh. 14 - Prob. 34QPCh. 14 - Prob. 35QPCh. 14 - Prob. 36QPCh. 14 - Prob. 37QPCh. 14 - Prob. 38QPCh. 14 - Prob. 39QPCh. 14 - Prob. 40QPCh. 14 - Prob. 41QPCh. 14 - Prob. 42QPCh. 14 - Prob. 43QPCh. 14 - Prob. 44QPCh. 14 - Prob. 45QP
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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
- 62. Pressure of the Photosphere. The gas pressure of the photosphere changes substantially from its upper levels to its lower levels. Near the top of the photosphere, the temperature is about 4500 K and there are about 1.6 x 1016 gas particles per cubic centimeter. In the middle, the temperature is about 5800 K and there are about 1.0 x 10" gas particles per cubic centimeter. At the bottom of the photosphere, the temperature is about 7000 K and there are about 1.5 × 10" gas particles per cubic centimeter. Use the ideal gas law (Mathematical Insight 14.2) to compare the pressures of each of these layers; explain the reason for the trend that you find. How do these gas pressures compare with Earth's atmospheric pressure at sea level?arrow_forward21. While observing the Sun, you note a large number of sunspots. What can you conclude? This is a period of low solar activity. Earth's climate will be unusually cold. The Sun is less luminous than usual. There are likely to be an above average number of flares and prominences. The Sun's rotation is slower than average.arrow_forwardHow does energy makes its way from the nuclear core of the Sun to its atmosphere? Choose the correct order for each layer. → O radiative zone, convection zone, photosphere, chromosphere, transition region, corona O convection zone, radiative zone, chromosphere, photosphere, transition region, corona convection zone, radiative zone, photosphere, chromosphere, transition region, corona O radiative zone, convection zone, chromosphere, transition region, photosphere, corona O radiative zone, convection zone, chromosphere, photosphere, transition region, corona #m с d $ 4 e 30 f % 5 t g bo 6 M 7 & 7 h O u 8 9arrow_forward
- Why do the magnetic fields lines of the sun get warped? a. effects of the solar wind b. surface of the sun is cooler near the poles c. uneven fusion rates in the core d. equator rotates more rapidly than the polesarrow_forwardWhich of the following layers of the Sun can be seen with some type of telescope? Consider all forms of light, but do not consider neutrinos or other particles. (Give ALL correct answers in alphabetical order, i.e., B, AC, BCD...)A) Corona.B) Photosphere.C) Radiation Zone.D) Chromosphere.E) Convection Zone.F) Core.arrow_forwardWhat types of changes effect the Sun's energy output? Cycle 24 Sunspot Number (V2.0) Prediction (2016 10) 300 200 100 Cycle Cycle Cycle 22 23 24 1985 1990 1995 2000 2005 2010 2015 2020 Hathaway NASA/ARC O A. 11 year solar sunspot cycles change the amount of radiation given off by the Sun. O B. As the Sun rotates more energy is scattered to space and less is retained on the surface. O C. Cycles of solar flares and prominences heat and cool the layers below the Sun's surface. O D. Solar energy is affected by the core output of photons.arrow_forward
- 1. When will the Sun exhaust its supply of hydrogen and no longer maintain the same state of hydrostatic equilibrium that exists today? (Assume that the Sun will run out of hydrogen fuel in its core, due to inefficient mixing, after 5% of the Sun's current total hydrogen content is converted into helium.)arrow_forwardNeutrinos produced in the core of the Sun carry energy to its exterior. Is the mechanism for this energy transport conduction, convection, or radiation?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
- Table 15.1 indicates that the density of the Sun is 1.41 g/cm3. Since other materials, such as ice, have similar densities, how do you know that the Sun is not made of ice?arrow_forwardIf 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.)arrow_forwardWhy do sunspots look dark?arrow_forward
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