Understanding Our Universe
Understanding Our Universe
3rd Edition
ISBN: 9780393614428
Author: PALEN, Stacy, Kay, Laura, Blumenthal, George (george Ray)
Publisher: W.w. Norton & Company,
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Chapter 13, Problem 6QAP
To determine

The order of nuclear burning in evolving high mass stars.

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The diagram below shows an H-R diagram with life track of a 1-solar-mass star, with various stages labeled A through E. Temperature What will happen to the star after stage E? A. It will gain mass until it collapses under its own weight. B. It will begin burning carbon in its core. C. It will explode in a supernova. D. It will collapse to make a neutron star. E. It will eject a planetary nebula. Luminosity →
The triple-alpha process   a. controls the pulsations in Cepheid variable stars.   b. is the nuclear fusion of hydrogen to helium in massive stars.   c. is the process that produces the neutrinos we receive from the sun.   d. requires a temperature of about 5,000,000 K to operate.   e. fuses helium nuclei to make carbon and occurs during helium flash.
There is a mass–luminosity relation because   a. hydrogen fusion produces helium.   b. stars expand when they become giants.   c. stars support their weight by making energy.   d. the helium flash occurs in degenerate matter.   e. all stars on the main sequence have about the same radius.
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