21st Century Astronomy
6th Edition
ISBN: 9780393428063
Author: Kay
Publisher: NORTON
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Chapter 14.1, Problem 14.1ACYU
To determine
The meaning of hydrostatic equilibrium.
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Check out a sample textbook solutionStudents have asked these similar questions
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.
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
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
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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- How long does it take for energy produced in the Sun's core to reach the photosphere? A. a few seconds B. a few hours O C. a few years D. a few hundred years E. a few hundred thousand yearsarrow_forward2. 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_forwarda.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_forward
- 10. Show explicitly that if the Sun's photosphere were not ionized, its mean molecular mass would be u 1.25.arrow_forwardWhy are measurements of the Sun's 10.7 cm radio emission used to monitor the state of the solar cycle? Choose all correct answers. A. It provides a repeatable, objective measurement of solar activity B. It serves as a good proxy for EUV emissions C. It is measured from space, so it is not affected by clouds D. It can be used to predict the occurrence of coronal mass ejectionsarrow_forwardWhy 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_forward
- Describe the process as a photon (energy) created in the Sun's core makes its way out into space. Make sure to consider the different layers that the photon must pass through to reach the Sun's surface.arrow_forwardStep-by-step, explain how energy flows from the center of the Sun to Earth.arrow_forward1. 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_forward
- 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_forwardHow are neutrinos observed? a. by using a large tank of cleaning fluid buried deep in beneath Earth’s surface b. by using spectral observations c. by using a radio receiver d. by using a Schmidt-Cassegrain focus e. by using a magneto-hydrodynamic detectorarrow_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
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