College Physics
2nd Edition
ISBN: 9780134601823
Author: ETKINA, Eugenia, Planinšič, G. (gorazd), Van Heuvelen, Alan
Publisher: Pearson,
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Chapter 30, Problem 7CQ
To determine
The reason for the fact that neutrinos are not easily detected even though billions of them pass through every square centimeter of our body every second.
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The power output of the Sun is 4 × 1026 W.
Part (a) If 93 % of this is supplied by the proton-proton cycle, how many protons are consumed per second?
Part (b) How many neutrinos per second should be incident on every square meter of the Earth from this process? This huge number is indicative of how rarely a neutrino interacts, since large detectors observe very few per day.
The power output of the Sun is 4×10^26 W. (a) If 90% of this energy is supplied by the proton-proton chain, how many protons are consumed per second? (b) How many neutrinos per second should there be per square meter at the surface of Earth from this process?
Only part (b) is needed.
The probability of two protons tunneling in the Sun's core is Ptunnel 1010. This means that out of each
1010 pairs of protons, one pair tunnels successfully. Make an estimate showing that this probability can
account for the 1038 fusion reactions that take place each second in the Sun's core. Hint: Assume that
the Sun's core contains about 40% of its mass.
Chapter 30 Solutions
College Physics
Ch. 30 - Prob. 1RQCh. 30 - Prob. 2RQCh. 30 - Review Question 30.3 Using what you have learned...Ch. 30 - Prob. 4RQCh. 30 - Prob. 5RQCh. 30 - Prob. 1MCQCh. 30 - Prob. 2MCQCh. 30 - Prob. 3MCQCh. 30 - Prob. 4MCQCh. 30 - Prob. 5CQ
Ch. 30 - Prob. 6CQCh. 30 - Prob. 7CQCh. 30 - Prob. 8CQCh. 30 - Prob. 9CQCh. 30 - Prob. 10CQCh. 30 - Prob. 11CQCh. 30 - 12. What are the components of the Standard...Ch. 30 - Prob. 13CQCh. 30 - Prob. 14CQCh. 30 - Prob. 1PCh. 30 - Prob. 2PCh. 30 - Prob. 3PCh. 30 - Prob. 4PCh. 30 - Prob. 5PCh. 30 - 6. Use Newtonian circular motion concepts to show...Ch. 30 - Prob. 7PCh. 30 - A particle enters a cloud chamber from above...Ch. 30 - Prob. 9PCh. 30 - Prob. 10PCh. 30 - Prob. 11PCh. 30 - Prob. 12PCh. 30 - Prob. 13PCh. 30 - 14. * Make an analogy between the interactions of...Ch. 30 - Why are neutrinos difficult to detect?Ch. 30 - Prob. 16PCh. 30 - Prob. 17PCh. 30 - Prob. 18PCh. 30 - Prob. 19PCh. 30 - Prob. 20PCh. 30 - Prob. 21PCh. 30 - Prob. 22PCh. 30 - Prob. 23PCh. 30 - Prob. 24PCh. 30 - Prob. 25PCh. 30 - Prob. 26PCh. 30 - * What is inflation, and what eventually happened...Ch. 30 - Prob. 29PCh. 30 - Prob. 30PCh. 30 - Prob. 31PCh. 30 - * Our bodies contain significant amounts of...Ch. 30 - 33. * What is the evidence that a large proportion...Ch. 30 - Prob. 34PCh. 30 - 35. * What is the experimental evidence for dark...Ch. 30 - Prob. 36PCh. 30 - Prob. 37PCh. 30 - Prob. 38PCh. 30 - Prob. 39PCh. 30 - * An electron and a positron are traveling...Ch. 30 - Prob. 41GPCh. 30 - Prob. 42RPPCh. 30 - Prob. 43RPPCh. 30 - Prob. 44RPP
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- The 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_forwardA chain of nuclear reactions in the Suns core converts four protons into a helium nucleus. (a) What is the mass difference between four protons and a helium nucleus? (b) How much energy in MeV is released during the conversion of four protons into a helium nucleus?arrow_forwardHow is a neutrino different from a neutron? List all the ways you can think of.arrow_forward
- We saw that, on Earth, the number flux of solar neutrinos from the p-p chain is 6.7E10 s-1 cm-2. Other nuclear reactions in the Sun supplement this neutrino flux with a small additional flux of higher-energy neutrinos. A neutrino detector in Japan, named Super Kamiokande, consists of a tank of 50kton of water, surrounded by photomultiplier tubes. The tubes detect the flash of Cerenkov radiation emitted by a recoiling electron when a high-energy neutrino scatters on it. Calculate the detection rate for neutrino scattering in events per day, if 10-6 of the solar neutrinos have a high enough energy to be detected by this experiment, and each electron poses a scattering cross section=10-43 cm. Hint: Consider the density of neutrino targets "seen" by an individual electron, with a relative velocity of c between the neutrinos and the electron, to obtain the rate at which one electron interacts with the incoming neutrinos, and multiply by the total number of electrons (I've already done this:…arrow_forwardEnergy generation in the Sun arises because hydrogen nuclei fuse to form helium nuclei. Write down the reactions involved in the proton-proton chain. State which reaction in the chain controls the rate at which the full set of reactions proceeds and explain why this is the case. Given that the solar luminosity is L = 3.8 × 1026 W, the combined mass of four protons is 6.690 × 10−27 kg and the mass of one helium nucleus is 6.643 × 10−27 kg, estimate the number of helium nuclei that have been generated inside the Sun over its 4.6 × 109 year life time.arrow_forwardCalculate the nuclear binding energy for a helium-5 atom (isotopic mass = 5.012057 u), a sodium-22 atom (isotopic = 21.99443742 u), and a cobalt-60 atom (isotopic mass = 59.9338222 u) I will provide an example for this question. See the imagearrow_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_forwardWhat fraction of the total energy released goes into the kinetic energy of the proton? Express your answer as a percentage. Kp/Ktot=arrow_forwardThe fusion reaction shown is part of the proton-proton chain that occurs in the core of the sun. He р He He р Energy The products and reactants have the following properties: Hydrogen: m=1.007825u Helium 3: m=3.01603u Helium 4: m=4.00260u Conversion factors 1u-1.66056x10-27 kg = 931.494 MeV/c². Calculate the energy given off during this step of the reaction. Give your answer in MeV.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 sun releases 3.826 × 10 26 Joules of energy every second, how many fusion reactions does it take to produce this each second?arrow_forwardA "mad" scientist attempts to take a sample of Mercury-199 and bombard it with neutrons. The reaction creates a proton and Gold-199. His joy is short-lived when in a few days the radioactive Gold-199 reverts back to Mercury-199 emitting a single particle. What is the emitted particle? 1999 Au 199 ¹20Hg+? 80 000 0 a beta (-) particle ß- a proton; H+ an alpha particle; a a neutron; nºarrow_forward
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