Physics for Scientists and Engineers, 4th Ed + Masteringphysics: Chapters 1-38
4th Edition
ISBN: 9780136139263
Author: Douglas C. Giancoli
Publisher: PEARSON EDUCATION (COLLEGE)
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2 protons released in what step of solar nuclear fusion?
a. step 1
b. step 2
c. none of the steps
d. step 3
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.
The proton – proton cycle responsible for the Sun’s 3.84 x 1026 W power output yields about 26.7 MeV of energy for every four protons that are fused into a helium nucleus. Determine (a) the energy in joules released during each proton – proton cycle fusion reaction, (b) the number of proton – proton cycles occurring per second in the Sun, and (c) the change in the Sun’s mass each second due to this energy release.
Chapter 42 Solutions
Physics for Scientists and Engineers, 4th Ed + Masteringphysics: Chapters 1-38
Ch. 42.1 - Prob. 1AECh. 42.3 - Prob. 1BECh. 42.4 - Return to the first Chapter-Opening Question, page...Ch. 42.4 - Prob. 1DECh. 42.6 - Prob. 1EECh. 42 - Prob. 1QCh. 42 - Prob. 2QCh. 42 - Prob. 3QCh. 42 - Why are neutrons such good projectiles for...Ch. 42 - Prob. 5Q
Ch. 42 - Prob. 6QCh. 42 - Prob. 7QCh. 42 - Prob. 8QCh. 42 - Prob. 9QCh. 42 - Prob. 10QCh. 42 - Prob. 11QCh. 42 - Why would a porous block of uranium be more likely...Ch. 42 - Prob. 13QCh. 42 - Prob. 14QCh. 42 - Prob. 15QCh. 42 - Prob. 16QCh. 42 - Prob. 17QCh. 42 - Prob. 18QCh. 42 - Prob. 19QCh. 42 - Prob. 20QCh. 42 - Prob. 21QCh. 42 - Prob. 22QCh. 42 - Prob. 23QCh. 42 - Prob. 24QCh. 42 - Prob. 25QCh. 42 - How might radioactive tracers be used to find a...Ch. 42 - Prob. 1PCh. 42 - Prob. 2PCh. 42 - Prob. 3PCh. 42 - Prob. 4PCh. 42 - Prob. 5PCh. 42 - Prob. 6PCh. 42 - Prob. 7PCh. 42 - Prob. 8PCh. 42 - Prob. 9PCh. 42 - Prob. 10PCh. 42 - Prob. 11PCh. 42 - Prob. 12PCh. 42 - Prob. 13PCh. 42 - Prob. 14PCh. 42 - Prob. 15PCh. 42 - Prob. 16PCh. 42 - Prob. 17PCh. 42 - Prob. 18PCh. 42 - (I) What is the effective cross section for the...Ch. 42 - Prob. 20PCh. 42 - Prob. 21PCh. 42 - Prob. 22PCh. 42 - Prob. 23PCh. 42 - Prob. 24PCh. 42 - Prob. 25PCh. 42 - Prob. 26PCh. 42 - Prob. 27PCh. 42 - Prob. 28PCh. 42 - Prob. 29PCh. 42 - Prob. 30PCh. 42 - Prob. 31PCh. 42 - Prob. 32PCh. 42 - Prob. 33PCh. 42 - Prob. 34PCh. 42 - Prob. 35PCh. 42 - Prob. 36PCh. 42 - Prob. 37PCh. 42 - Prob. 38PCh. 42 - Prob. 39PCh. 42 - Prob. 40PCh. 42 - Prob. 41PCh. 42 - Prob. 42PCh. 42 - Prob. 43PCh. 42 - Prob. 44PCh. 42 - Prob. 45PCh. 42 - Prob. 46PCh. 42 - Prob. 47PCh. 42 - Prob. 48PCh. 42 - Prob. 49PCh. 42 - Prob. 50PCh. 42 - Prob. 51PCh. 42 - Prob. 52PCh. 42 - Prob. 53PCh. 42 - Prob. 54PCh. 42 - Prob. 55PCh. 42 - Prob. 56PCh. 42 - Prob. 57PCh. 42 - Prob. 58PCh. 42 - Prob. 59PCh. 42 - Prob. 60PCh. 42 - Prob. 61PCh. 42 - Prob. 62PCh. 42 - Prob. 63PCh. 42 - Prob. 64PCh. 42 - Prob. 65GPCh. 42 - Prob. 66GPCh. 42 - Prob. 67GPCh. 42 - Prob. 68GPCh. 42 - Prob. 69GPCh. 42 - Prob. 70GPCh. 42 - Prob. 71GPCh. 42 - Prob. 72GPCh. 42 - Prob. 73GPCh. 42 - Prob. 74GPCh. 42 - Prob. 75GPCh. 42 - Prob. 76GPCh. 42 - Prob. 77GPCh. 42 - Prob. 78GPCh. 42 - Prob. 79GPCh. 42 - Prob. 80GPCh. 42 - Prob. 81GPCh. 42 - Prob. 82GPCh. 42 - Prob. 83GPCh. 42 - Prob. 84GPCh. 42 - Prob. 85GPCh. 42 - Prob. 86GPCh. 42 - Prob. 87GPCh. 42 - Prob. 88GP
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- What conditions are required before proton-proton chain fusion can start in the Sun?arrow_forwardSuppose the proton-proton cycle in the Sun were to slow down suddenly and generate energy at only 95% of its current rate. Would an observer on Earth see an immediate decrease in the Sun’s brightness? Would she immediately see a decrease in the number of neutrinos emitted by the Sun?arrow_forwardWhy is a higher temperature required to fuse hydrogen to helium by means of the CNO cycle than is required by the process that occurs in the Sun, which involves only isotopes of hydrogen and helium?arrow_forward
- About 2% of the energy generated in the Sun’s core by the p-p reaction is carried out of the Sun by neutrinos. Is the energy associated with this neutrino flux equal to, greater than, or less than the energy radiated from the Sun’s surface as electromagnetic radiation?arrow_forwardWhat were the most common nuclear reactions involved in the formation of elements within the first second and after the big explosion? Give examples of each type of nuclear reaction.arrow_forwardThe sun generates its energy through nuclear fusion, making helium from hydrogen. The main process by which this happens, called the proton-proton chain, goes as follows: Two protons come together to create deuterium, a positron, a neutrino, and energy: p + p ⟶ D + e+ + ν + energy The deuterium fuses with another proton to make 3He: D + p ⟶ 3He + energy Fianlly, 4He is produced by fusing two 3He nuclei together: 3He + 3He ⟶ 4He + p + p + energy What is the total energy released during the creation of one 4He nucleus? Give your answer in MeV, and remember that you need to make two 3He nuclei in the process. Be sure to use at least five significant figures for your masses, but your final answer should have three or four sig figs.arrow_forward
- The total energy output from the Sun of around 3.8 x 1026 joules per second, what is the mass of elements consumed in order to produce this amount of energy?arrow_forwardCalculate and compare the energy released by (a) the fusion of 1.0 kg of hydrogen deep within the Sun and (b) the fission of 1.0 kg of 235U in a fission reactor.arrow_forwardExplain the fusion reaction that occurs in the Sun?arrow_forward
- The sun radiates energy at the rate of 3.85 × 1026 W. Suppose the net reaction 4p + 2e− → α + 2υe + 6γ accounts for all the energy released. Calculate the number of protons fused per second. Note: Recall that an alpha particle is a helium-4 nucleus.arrow_forwardThe 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_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
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