Universe
Universe
11th Edition
ISBN: 9781319039448
Author: Robert Geller, Roger Freedman, William J. Kaufmann
Publisher: W. H. Freeman
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Chapter 19, Problem 6CC
To determine

The safety valve for the main-sequence star’s nuclear reactions and the reason for its absence in the red giant in which the core is supported by degenerate-electron pressure.

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We will take a moment to compare how brightly a white dwarf star shines compared to a red giant star. For the sake of this problem, let's assume a white dwarf has a temperature around 10,000 K and a red giant has a temperature around 5,000 K. As for their stellar radiatin, the white dwarf has a radius about 1/100th that of the Sun, and a red giant has a radius around 100 times larger than the Sun. With this in mind, how does the luminosity of a red giant star compare to that of a white dwarf (Hint: do not try to enter all of these numbers into the luminosity equation {it won't go well}; instead, remember that you are only interested in the ratio between the two, so all common units and components can be divided out)? Please enter your answer in terms of the luminosity of the red giant divided by the luminosity of the white dwarf and round to two significant figures. Also, please avoid using commas in your answer.
A red giant that was originally a 9.5MSun main-sequence star loses a solar mass in 100,000 years via a superwind. What is this mass loss rate in units of solar masses per year? (the answer is not 0.000095 solar masses per year).     Additionally, at this mass loss rate, what will the red giant's mass be after 0.5 million years? (Enter your answer as a multiple of MSun.)
If a giant molecular cloud has a mass of 2.0 ✕ 1035 kg, and it converts 8 percent of its mass into stars during a single encounter with a shock wave, how many stars can it make? Assume the stars each contain 1 solar mass. (Hint: The mass of the Sun is 1.99 ✕ 1030 kg.)
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