Universe: Stars And Galaxies
6th Edition
ISBN: 9781319115098
Author: Roger Freedman, Robert Geller, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 16, Problem 60Q
To determine
(a)
The advantages and disadvantages of observing the Sun from Space.
To determine
(b)
The advantages and disadvantages of observing the Sun from Earth’s South Pole.
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Earth's daylight surface disk absorbs about 1036 W per m2 from the Sun. Using 6400 km for the Earth's radius, how much of this radiative power is emitted by each square meter of the spherical Earth? Hint: Compare the ratio of the disk area to the spherical surface area.
Why 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 ejections
What physics theory related to the solar energy? State and explain.
Chapter 16 Solutions
Universe: Stars And Galaxies
Ch. 16 - Prob. 1QCh. 16 - Prob. 2QCh. 16 - Prob. 3QCh. 16 - Prob. 4QCh. 16 - Prob. 5QCh. 16 - Prob. 6QCh. 16 - Prob. 7QCh. 16 - Prob. 8QCh. 16 - Prob. 9QCh. 16 - Prob. 10Q
Ch. 16 - Prob. 11QCh. 16 - Prob. 12QCh. 16 - Prob. 13QCh. 16 - Prob. 14QCh. 16 - Prob. 15QCh. 16 - Prob. 16QCh. 16 - Prob. 17QCh. 16 - Prob. 18QCh. 16 - Prob. 19QCh. 16 - Prob. 20QCh. 16 - Prob. 21QCh. 16 - Prob. 22QCh. 16 - Prob. 23QCh. 16 - Prob. 24QCh. 16 - Prob. 25QCh. 16 - Prob. 26QCh. 16 - Prob. 27QCh. 16 - Prob. 28QCh. 16 - Prob. 29QCh. 16 - Prob. 30QCh. 16 - Prob. 31QCh. 16 - Prob. 32QCh. 16 - Prob. 33QCh. 16 - Prob. 34QCh. 16 - Prob. 35QCh. 16 - Prob. 36QCh. 16 - Prob. 37QCh. 16 - Prob. 38QCh. 16 - Prob. 39QCh. 16 - Prob. 40QCh. 16 - Prob. 41QCh. 16 - Prob. 42QCh. 16 - Prob. 43QCh. 16 - Prob. 44QCh. 16 - Prob. 45QCh. 16 - Prob. 46QCh. 16 - Prob. 47QCh. 16 - Prob. 48QCh. 16 - Prob. 49QCh. 16 - Prob. 50QCh. 16 - Prob. 51QCh. 16 - Prob. 52QCh. 16 - Prob. 53QCh. 16 - Prob. 54QCh. 16 - Prob. 55QCh. 16 - Prob. 56QCh. 16 - Prob. 57QCh. 16 - Prob. 58QCh. 16 - Prob. 59QCh. 16 - Prob. 60Q
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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
- Solar scientists want to measure the temperature inside the sun by sending in probes. Imagine that temperature increases by 1 million◦C for every 10,000 km below the surface. A probe that can handle a temperature of x million degrees costs x³ million dollars. a. How much would it cost to measure the temperature 10,000 km down? b. How much would it cost to measure the temperature 100,000 km down? c. How much would it cost to measure the temperature 200,000 km down?arrow_forwardChapter #8, Question #2: Use eqn. 8.4 (F = σT4) to show why the total flux of solar radiant energy is about 105 times greater than that from the Earth.arrow_forwardEarth's daylight surface disk absorbs about 1047 W per m2 from the Sun. Using 6400 km for the Earth's radius, how much of this radiative power is emitted by each square meter of the spherical Earth? (Compare ratio of disk area to spherical surface area)arrow_forward
- What is the value of the IR transmission factor (f) for a Venus-like planet, if the measured average surface temperature is 706 K? Assume the following values for the planet: E, = 2.60x10³ W m² and a = 0.71. Would the average temperature increase or decrease if f decreased?arrow_forward2. Plasma oscillations in the ionosphere. The plasma density in the lower ionosphere has been measured during satellite reentry to be about a) 10¹8 m-³ at 50 km altitude, b) 10¹7 m-³ at 70 km and c) 10¹4 m²³ at 85 km. Use the formula for the electron plasma frequency to compute its numerical value for each of these three altitudes, AND state (we'll address this quantitatively later, when we get to EM wave propagation in plasmas) why the ionosphere is a relevant consideration for radio communications both on earth and between earth and interplanetary spacecraft.arrow_forwardEarths daylight surface disk absorbs about 1045 W per m2 from the Sun. Using 6400 km for the Earths radius, how much of this radiative power is emitted by each square meter of the spherical Earth ?arrow_forward
- Our Sun has a surface temperature of about 5800 K. Find the emitted power per square meter of peak intensity for a similar star with 4600 K that emits thermal radiation. Express your answer in scientific notation and with three significant figures.arrow_forward. How big would a square solar sail need to be in order for sunlight to exert a 12 N force on it (use 1,100 W/m² as the intensity of the sunlight).arrow_forwardWrite the factors that influence Ionization energy and explain any three of them.arrow_forward
- Q26-A(i). Define solar constant. Explain a process which converts light energy into electricity.arrow_forwardK What is the wavelength (in nm) of the most intense radiation emitted from the surface of Mercury at high noon? (Hint: Use Wien's law, Amax = 2.90 x 10° m: K %3D T (in K) nm In which band of the electromagnetic spectrum is that wavelength? (Hint: Examine the following figure.) Visible light Short wavelengths Long wavelengths 4 x 107 5x 107 6x 107 7x 10meters (400 nm) (500 nm) (600 nm) /(700 nm) Wavelength (meters) 10 12 10 10 10 104 102 1 102 104 Gamma- ray Ultra- violet Micro- Radio X-ray Infrared wave UHF VHF FM AM a Opaque Visual window Radio window Transparent Short Wavelength Long b O gamma-ray O X-ray O ultraviolet O visual O infrared O microwave O radio оооо о оо Opacity of Earth's atmospherearrow_forwardThe Sun has a radius of about 700,000 km and a surface temperature of 5800 K. Assuming it is a perfect blackbody (an emissivity of 1), what is the rate of energy radiated (in W) from the surface of the Sun? (Hint: the surface area of a sphere is 4πR2; enter your answer in scientific notation, 1.23E12 means 1.23 * 1012).arrow_forward
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