Modern Physics
3rd Edition
ISBN: 9781111794378
Author: Raymond A. Serway, Clement J. Moses, Curt A. Moyer
Publisher: Cengage Learning
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Chapter 15, Problem 36P
To determine
Total number of neutrinos passed through a human.
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How much energy (in x 1016 Joule) does the Sun burn 1 kg of hydrogen fuel in a nuclear reaction?
A standard nuclear power plant generates 3.0 GWGW of thermal power from the fission of 235U235U. Experiments show that, on average, 0.19 uu of mass is lost in each fission of a 235U235U nucleus.
How many kilograms of 235U235U undergo fission each year in this power plant?
Express your answer in kilograms per year.
The half-lives of 235U and 238U are 7.04 × 108 years and 4.47 × 109 years, respectively, and the present abundance ratio is 238U>235U 5 137.7. It is thought that their abundance ratio was 1 at some time before our earth and solar system were formed about 4.5 × 109 years ago. Estimate how long ago the supernova occurred that supposedly produced all the uranium isotopes in equal abundance, including the two longest lived isotopes, 238U and 235U.
Chapter 15 Solutions
Modern Physics
Ch. 15.6 - Prob. 2ECh. 15.7 - Prob. 3ECh. 15 - Prob. 1QCh. 15 - Prob. 2QCh. 15 - Prob. 3QCh. 15 - Prob. 4QCh. 15 - Prob. 5QCh. 15 - Prob. 6QCh. 15 - Prob. 7QCh. 15 - Prob. 9Q
Ch. 15 - Prob. 10QCh. 15 - Prob. 11QCh. 15 - Prob. 12QCh. 15 - Prob. 14QCh. 15 - Prob. 15QCh. 15 - Prob. 16QCh. 15 - Prob. 17QCh. 15 - Prob. 18QCh. 15 - Prob. 1PCh. 15 - Prob. 2PCh. 15 - Prob. 3PCh. 15 - Prob. 4PCh. 15 - Prob. 5PCh. 15 - Prob. 6PCh. 15 - Prob. 7PCh. 15 - Prob. 8PCh. 15 - Prob. 9PCh. 15 - Prob. 10PCh. 15 - Prob. 11PCh. 15 - Prob. 12PCh. 15 - Prob. 13PCh. 15 - Prob. 14PCh. 15 - Prob. 15PCh. 15 - Prob. 16PCh. 15 - Prob. 17PCh. 15 - Prob. 18PCh. 15 - Prob. 19PCh. 15 - Prob. 20PCh. 15 - Prob. 21PCh. 15 - Prob. 22PCh. 15 - Prob. 23PCh. 15 - An unstable particle, initially at rest, decays...Ch. 15 - Prob. 25PCh. 15 - Prob. 26PCh. 15 - Prob. 27PCh. 15 - Prob. 28PCh. 15 - Prob. 29PCh. 15 - Prob. 30PCh. 15 - Prob. 31PCh. 15 - Prob. 32PCh. 15 - Prob. 33PCh. 15 - Prob. 34PCh. 15 - Prob. 35PCh. 15 - Prob. 36P
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- The Sun and all Main Sequence stars derive their luminosity by fusing hydrogen to helium; in particular 4 1H ® 1 4He + Energy (photons) The mass of a proton is 1.0078 AMU, while the mass of a helium nucleus is 4.0026 AMU. a) How much mass is ``lost'' (in AMU and kg) in fusing four H atoms to one helium? This is called the mass defect. b) Mass isn't really lost, of course. It is converted to energy via E=mc2. How much energy in joules (J) is liberated in a single reaction? c) How many reactions per second are required to account for the entire luminosity of the Sun?arrow_forwardThe power output of the Sun is 41026W. (a) If 90% of this is supplied by the protonproton cycle, how many protons are consumed per second? (b) How many neutrinos per second should there be per square meter at the Earth from this process? This huge number is indicative of how rarely a neutrino interacts, since large detectors observe very few per day.arrow_forwardThe primary decay mode for the negative pion is +v . (a) What is the energy release in MeV in this decay? (b) Using conservation of momentum, how much energy does each of the decay products receive, given the is at rest when it decays? You may assume the muon antineutrino is massless and has momentum p = E/c , just like a photon.arrow_forward
- (a) What is the uncertainty in the energy released in the decay of a due to its short lifetime? (b) Is the uncertainty in 1his energy greater than or lees than the uncertainty in the mass of the tau neutrino? Discuss the source of the uncertainty.arrow_forwardUsing data from Potential Energy of a System (http://cnx.org/content/m58312/latest/#fs-id1165036086155) , calculate the amount of mass converted to energy by the fusion of 1.00 kg of hydrogen. (b) What is the ratio of mass destroyed to the original mass, (c) How does this compare with for the fission of 1.00 kg of uranium?arrow_forwardThe primary decay mode for the negative pion is π− → μ− + ν-μ . (a) What is the energy release in MeV in this decay? (b) Using conservation of momentum, how much energy does each of the decay products receive, given the π− is at rest when it decays? You may assume the muon antineutrino is massless and has momentum p = E / c , justlike a photon.arrow_forward
- Suppose you are designing a proton decay experiment and you can detect 50 percent of the proton decays in a tank of water. (a) How many kilograms of water would you need to see one decay per month, assuming a lifetime of 1031 y ?(b) How many cubic meters of water is this? (c) If the actual lifetime is 1033 y , how long would you have to wait on anaverage to see a single proton decay?arrow_forwardThe Sun's mass is1.989 ×10^8 and it radiates at a rate of 3.827×10^23 kW. a) From this data, assuming it converts all its mass into energy, what is the estimate the lifetime of the Sun? b) Theoretical calculations predict the Sun's lifetime (in its current stage) to be about 5 billion years. During that time, what percentage of its mass will it lose?arrow_forwardSuppose that a tau neutrino and a tau antineutrino, both of which are just barely moving, encounter each other in space and completely annihilate to form two photons of equal energy. In view of the uncertainty about the mass of the tau neutrino (<18.2 MeV/c2), what is the shortest wavelength lamda0 of light that could be emitted by the annihilation? lamda0 = ? m Would the light be visible to the human eye?arrow_forward
- What is the rest energy (in joules) of a subatomic particle whose (rest) mass is 6.7×10−31 kg? How many MeV’s of energy is this?arrow_forwardSuppose you are designing a proton decay experiment and you can detect 50 percent of the proton decays in a tank of water. (a) How many kilograms of water would you need to see one decay per month, assuming a lifetime of 1031 y ? (b) How many cubic meters of water is this? (c) If the actual lifetime is 1033 y , how long would you have to wait on an average to see a single proton decay?arrow_forwardIf our Sun (mass = 1.99××103030 kg, radius = 6.96××1088 m) were to collapse into a neutron star (an object composed of tightly packed neutrons with roughly the same density as neutrons within a nucleus, ρnucleusρnucleus = 2.3××101717 kg/m33), what would the new radius of our “neutron-sun” be?arrow_forward
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