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 40QAP
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Energy released from fusing
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The Sun is powered by releasing hydrogen to helium. Through either the proton-proton chain or the CNO cycle, the basic reaction is 4 1H morph into 1 4He, releasing nuclear binding energy (and losing mass) in the process. The mass of one proton 1H is 1.6726 x 10-24 gm and the mass of one helium nucleus 4He is 6.6447 x 10-24 gm.
What is the mass difference in gm between 4 protons and one helium nucleus? Calculate the ratio of the mass difference to the original mass of the 4 protons as a comparison.
Chapter 13 Solutions
Understanding Our Universe
Ch. 13.1 - Prob. 13.1CYUCh. 13.2 - Prob. 13.2CYUCh. 13.3 - Prob. 13.3CYUCh. 13.4 - Prob. 13.4CYUCh. 13.5 - Prob. 13.5CYUCh. 13.6 - Prob. 13.6CYUCh. 13 - Prob. 1QAPCh. 13 - Prob. 2QAPCh. 13 - Prob. 3QAPCh. 13 - Prob. 4QAP
Ch. 13 - Prob. 5QAPCh. 13 - Prob. 6QAPCh. 13 - Prob. 7QAPCh. 13 - Prob. 8QAPCh. 13 - Prob. 9QAPCh. 13 - Prob. 10QAPCh. 13 - Prob. 11QAPCh. 13 - Prob. 12QAPCh. 13 - Prob. 13QAPCh. 13 - Prob. 14QAPCh. 13 - Prob. 15QAPCh. 13 - Prob. 16QAPCh. 13 - Prob. 17QAPCh. 13 - Prob. 18QAPCh. 13 - Prob. 19QAPCh. 13 - Prob. 20QAPCh. 13 - Prob. 21QAPCh. 13 - Prob. 22QAPCh. 13 - Prob. 23QAPCh. 13 - Prob. 24QAPCh. 13 - Prob. 26QAPCh. 13 - Prob. 27QAPCh. 13 - Prob. 28QAPCh. 13 - Prob. 29QAPCh. 13 - Prob. 30QAPCh. 13 - Prob. 31QAPCh. 13 - Prob. 32QAPCh. 13 - Prob. 33QAPCh. 13 - Prob. 35QAPCh. 13 - Prob. 36QAPCh. 13 - Prob. 37QAPCh. 13 - Prob. 38QAPCh. 13 - Prob. 39QAPCh. 13 - Prob. 40QAPCh. 13 - Prob. 41QAPCh. 13 - Prob. 43QAPCh. 13 - Prob. 44QAPCh. 13 - Prob. 45QAP
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- The nuclear process for fusing helium into carbon is often called the “triple-alpha process.” Why is it called as such, and why must it occur at a much higher temperature than the nuclear process for fusing hydrogen into helium?arrow_forwardWhy is fission not an important energy source in the Sun?arrow_forwardWhat conditions are required before proton-proton chain fusion can start in the Sun?arrow_forward
- Someone suggests that astronomers build a special gamma-ray detector to detect gamma rays produced during the proton-proton chain in the core of the Sun, just like they built a neutrino detector. Explain why this would be a fruitless effort.arrow_forwardWhy is it important to measure neutrinos and positrons coming from the sun?arrow_forwardAssume that the core of the Sun has one-eighth of the Sun’s mass and is compressed within a sphere whose radius is one-fourth of the solar radius.Assume further that the composition of the core is 31% hydrogen by mass and that essentially all the Sun’s energy is generated there. If the Sun continues to burn hydrogen at the current rate of 6.33E11 kg/s, how long, in years, will it be before the hydrogen is entirely consumed? Mass of the Sun is 2.0x1030 kg.arrow_forward
- The energy flux carried by neutrinos from the Sun is estimated to be on the order of 0.400 W/m2 at the Earth's surface. Estimate the fractional mass loss of the Sun over 1.0 109 yr due to the emission of neutrinos. The mass of the Sun is 1.989 1030 kg. The Earth–Sun distance is 1.496 1011 m. m msun =arrow_forwardBoth the CNO cycle and the proton–proton chain combine 4 H nuclei to produce 1 He nucleus. Would those two processes release the same amount of energy per He nucleus produced?arrow_forwardOne of the end stages of stellar life is a neutron star, where matter collapses and electrons combine with protons to form neutrons. Some liken neutron stars to a single gigantic nucleus. Calculate the radius in meters of a neutron star with a mass 3.34 x 1030 kg, treating it as a giant nucleus. Consider the mass of a nucleon 1.675 x 10-27 kg. Your answer should be in the form of N x 104 years.arrow_forward
- The energy flux carried by neutrinos from the Sun is estimated to be on the order of 0.400 W/m2 at the Earth’s surface. Estimate the fractional mass loss of the Sun over 109 yr due to the emission of neutrinos. The mass of the Sun is 1.989 × 1030 kg. The Earth–Sun distance is equal to 1.496 × 1011 m.arrow_forwardIf the nuclear fusion reaction of converting 4 H → He occurs at an efficiency of 0.7%, and that mass is converted into energy according to the equation E = mc2, then estimate the Main Sequence lifetime of the Sun (spectral type G2) in years if the Sun (⊙) has a surface luminosity L⊙ = 3.839°ø1033 erg. Assume the Sun’s core (10% of the total mass) is converted from H into He. The Sun’s mass is M⊙ = 1.9891 °ø 1033 g.arrow_forwardWhat is the net result of the nuclear process in the Sun's core? Group of answer choices Four helium fuse to form hydrogen Four hydrogen fuse to form deuterium. Helium fissions to form hydrogen. Four hydrogen fuse to form helium.arrow_forward
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