21st Century Astronomy
6th Edition
ISBN: 9780393428063
Author: Kay
Publisher: NORTON
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Question
Chapter 14, Problem 1QP
To determine
The confirmation for the physical model of the interior of sun.
Expert Solution & Answer
Answer to Problem 1QP
Option (a)
Explanation of Solution
Sun’s interior comprises of zones defined by the means of energy transportation in that region. By means of
Multiple layers of the sun are characterized by pressure, density, and temperature. Sun’s interior gets directly probed by Neutrinos and seismic vibrations. The model of Sun’s interior has been tested by helio-seismology.
.
Conclusion:
Therefore, option (a) is correct.
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Students have asked these similar questions
The sunspot cycle affects
I. the latitude at which sunspots are visible at a given time.
II. the number of sunspots that are visible at a given time.
III. the rotation rate of the sun’s equator at a given time.
IV. the magnetic polarity of the sunspots at a given time.
a.
I & II
b.
I & IV
c.
II & III
d.
I, II & III
e.
I, II, & IV
The sun has a radius of 6.959 × 108 m and a surface temperature of 5.81 x 10° K.
When the sun radiates at a rate of 3.91 x 1026 W and is a perfect emitter. What is
the rate of energy emitted per square meter? Stefan-Boltzmann constant is 5.67 x
10-8 J/s-m2 K4
a)
5.6 x 107 W/m2
b) 12.8 x 107 W/m2
c)
6.4 x 107 W/m2
25.6 x 107 W/m2
5.6 x 1017 W/m2
What 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.
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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- 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_forwardFor several hundred years, astronomers have kept track of the number of solar flares, or sunspots which occur on the surface of the sun. The number of sunspots counted varies periodically from a minimum of about 10 per year to a maximum of about 110 per year. Between the maximum that occurred in the years 1750 and 1948, there were 18 completed cycles. A.) What is the period of the sunspot cycle? B.) Assume that the number of sunspots varies sinusoidally with the year. Sketch a graph of two sun spot cycles, starting in 1948. C.) Write an equation expressing the number of sunspots per year in terms of the year. D.) what is the first year after 2000 in which the number of sunspots will be about 35? A maximum?arrow_forwardThe 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 corearrow_forward
- 2. Assume that the entire luminosity of the Sun is due to the PP chain reaction. The complete PP chain reaction converts 4 hydrogen nuclei into 1 helium nucleus, according to the following reaction: 4 H - He + 2e* + 2v. a. Estimate the amount of energy released by one complete reaction. b. Estimate how many of these reactions occur per second in the Sun, and how many neutrinos the Sun produces each second. c. Estimate the flux of neutrinos (in v's s' cm?) passing through the Earth.arrow_forward10. Show explicitly that if the Sun's photosphere were not ionized, its mean molecular mass would be u 1.25.arrow_forward7 Why do sunspots look dark? they are holes in the photosphere through which the cooler interior of the Sun is visible O they are much cooler than the rest of the surface of the Sun due to changes in the Sun's magnetic field O they are patches of the photosphere that burn up, creating ashes that look dark O Sunspots are regions in the upper chromosphere where there is a lot of coronium, which absorbs light O they are much hotter than the surrounding area, so their emission peaks in UV wavelengths, which our eyes cannot see с C 5 O 0 D "Aarrow_forward
- Q. How will our sun actually die? Pls answer in 2-3 sentences. Thank You!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_forward13 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 Sunarrow_forward
- a.Calculate the mass loss rate of the Sun M˙ due to the solar wind flow. Assume averageproperties of the solar wind of number density 6 protons cm−3, and a flow speed of 450 kms−1. Express your answer in units of both kg per year, and solar masses per year. b.Suppose the solar wind flow is perfectly radial. Calculate the expected rate of change ofsolar rotation frequency dω/dt at the present time, based on conservation of angular momentum. Give your answer in units of rad s−1 y−1(i.e., radians per second per year) and alsoin terms of fractional change per year, i.e., 1/ωdω/dt .Use a current solar rotation period of P = 25.38 days to calculate the current angularfrequency of rotation ω. The moment of inertia of a uniform sphere is 2/5 MR2. You canassume that the radius of the Sun is approximately constant, and the change in its momentof inertia due to the solar wind is only due to the mass loss. c.By observing the rotation period of stars similar to the Sun, it is inferred that their…arrow_forwardIt what layer of the sun does fusion occur? a. core b. radiative zone c. corona d. convective zonearrow_forward62. 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_forward
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