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ISBN: 9781111794378
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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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Twelve electron antineutrinos from Supernova 1987A were detected by the Kamiokande neutrino detector in Japan. This experiment consisted of a tank filled with 3 kton of water, and surrounded by photomultiplier tubes. The photomultipliers detect the Cerenkov radiation emitted by a recoiling positron that is emitted after a proton absorbs an antineutrino from the supernova.
Estimate how many people on Earth could have perceived a flash of light, due to the Cerenkov radiation produced by the same process, when an antineutrino from the supernova traveled through their eyeball. Assume that eyeballs are composed primarily of water, each weighs about 10 g, and that the Earth’s population was 5 billion in 1987.
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
=
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:…
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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- Most of the energy released in the collapse of a massive star to a neutron star (a core collapse supernova) is in the form of neutrinos. If the just-formed neutron star has a mass M = 1.4M⊙ and a radius R = 10 km, estimate the mean nucleon density, in cm−3. Find the mean free path, in cm, of a neutrino inside the neutron star, assuming the density you found and a cross section for scattering of neutrinos on neutrons of σνn = 10−42 cm2.arrow_forwardCalculate the energy Er, in megaelectronvolts (MeV), released in the following nuclear fission reaction: Cm(250) + n → Se(92) + Sm(153) + 6n The atomic masses are Cm(250)=250.078357 u, Se(92)=91.949926 u, and Sm(153)=152.922097 u. Er = ? MeVarrow_forwardThe 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.arrow_forward
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- A π meson (rest mass 135MeV/c2) moving through the laboratory at a speed of 0.998c decays into two gamma-ray photons. The two photons have equal energies Eγ and move at equal angles ? on opposite sides of the direction of motion of the original π meson. Calculate Eγ and θ.arrow_forward3 a) The three neutrino mass eigenstates are labelled m1, m2 and m3. Experiments have determined that Am² = m² – mị = 7.5 x 10-5 eV² and |Am22| = |m3 – m3| 2.5 x 10-3 eV². Calculate the smallest possible values of mı, m2 and m3 for: (i) the normal mass hierarchy. (ii) the inverted mass hierarchy. b) When L is expressed in km, E, in GeV and Am2 in eV², the two-flavour mixing formula for the probability of a v neutrino appearing a distance L later as a ve neutrino is Am²[eV*] L[km] E„[GeV] P(v, → v.) = sin²(20) sin? ( 1.27 where 0 is the neutrino mixing angle, Am² is the difference in the squared masses of the neutrino eigenstates and E, is the neutrino energy. The terms in square brackets denote the parameters' units. Assuming E, = 1.3 GeV, Am² = 2.5x10-3 eV² and sin 0 = /3/2, sketch P(v, → ve) and P(v → vµ) as a function of L in the range 0< L[km] < 3000. %3D For a long baseline experiment designed to detect muon-neutrinos with the param- eters E, distance L where the muon-neutrino…arrow_forwardThe 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_forward
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