Essential University Physics: Volume 2 (3rd Edition)
3rd Edition
ISBN: 9780321976420
Author: Richard Wolfson
Publisher: PEARSON
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Chapter 39, Problem 31E
To determine
The estimation of volume of the 50,000 tons of water used in Super Kamiokande experiment.
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=
U is for Uranium. Natural uranium consists of 235U (percent abundance P₁ = 0.7300%, A₁ =
3.12 x 10-¹7 [s-¹]) and 233U (percent abundance P₂ = 99.27%, 2₂ = 4.92 × 10-¹8 [s-¹]).
Consider the time when Earth was formed 4.5 billion years ago.
Setup the time dependence of percent abundance of the two uranium isotopes. Use №₁ and N₂
as current particle count of the isotopes (use №₁,0 and N₂,0 for the initial particle count back
when Earth was formed)
Then, Compute for the initial percent abundance of each uranium isotopes when the Earth was
formed.
Needs Complete typed solution with 100 % accuracy.
The photons that make up the cosmic microwave background were emitted about 380,000 years after the Big Bang. Today, 13.8
billion years after the Big Bang, the wavelengths of these photons have been stretched by a factor of about 1100 since they were
emitted because lengths in the expanding universe have increased by that same factor of about 1100.
Consider a cubical region of empty space in today's universe 1.00 m on a side, with a volume of 1.00 m³. What was the length
so of each side and the volume V of this same cubical region 380,000 years after the Big Bang?
So =
Vo =
Enter numeric value
Today the average density of ordinary matter in the universe is about 2.4 × 10-27 kg/m³. What was the average density po of
ordinary matter at the time that the photons in the cosmic microwave background radiation were emitted?
Po =
m
m³
kg/m³
Chapter 39 Solutions
Essential University Physics: Volume 2 (3rd Edition)
Ch. 39 - Prob. 1FTDCh. 39 - Prob. 2FTDCh. 39 - Prob. 3FTDCh. 39 - Prob. 4FTDCh. 39 - Prob. 5FTDCh. 39 - Prob. 6FTDCh. 39 - Prob. 7FTDCh. 39 - Prob. 8FTDCh. 39 - Name the fundamental force involved in (a) binding...Ch. 39 - Prob. 10FTD
Ch. 39 - Prob. 11FTDCh. 39 - Prob. 12FTDCh. 39 - Prob. 13FTDCh. 39 - Prob. 14FTDCh. 39 - Describe the origin of the cosmic microwave...Ch. 39 - Prob. 16FTDCh. 39 - Prob. 17FTDCh. 39 - The radiation that we observe as the cosmic...Ch. 39 - Prob. 19FTDCh. 39 - Prob. 20FTDCh. 39 - Prob. 21ECh. 39 - Prob. 22ECh. 39 - Prob. 23ECh. 39 - Prob. 24ECh. 39 - Prob. 25ECh. 39 - Prob. 26ECh. 39 - Prob. 27ECh. 39 - Prob. 28ECh. 39 - Prob. 29ECh. 39 - Prob. 30ECh. 39 - Prob. 31ECh. 39 - Prob. 32ECh. 39 - Prob. 33ECh. 39 - Prob. 34ECh. 39 - Prob. 35ECh. 39 - Prob. 36ECh. 39 - Prob. 37ECh. 39 - Prob. 38PCh. 39 - Prob. 39PCh. 39 - Prob. 40PCh. 39 - Prob. 41PCh. 39 - Prob. 42PCh. 39 - Prob. 43PCh. 39 - Prob. 44PCh. 39 - Prob. 45PCh. 39 - Prob. 46PCh. 39 - Prob. 47PCh. 39 - Prob. 48PCh. 39 - Prob. 49PCh. 39 - Prob. 50PCh. 39 - Prob. 51PCh. 39 - Prob. 52PCh. 39 - Prob. 53PCh. 39 - Prob. 54PCh. 39 - Prob. 55PCh. 39 - Prob. 56PCh. 39 - Prob. 57PCh. 39 - Prob. 58PCh. 39 - Prob. 59PCh. 39 - Prob. 60PCh. 39 - Prob. 61PPCh. 39 - Prob. 62PPCh. 39 - Prob. 63PPCh. 39 - Prob. 64PP
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- Vapor pressure of a pure component (Psat) can be computed from the correlation equations. Beattie et al.(1951) gives the following equation between 50.00 to 160.60 °C for neopentane: 1136.462 log10 pat = 3.901633 + 4.99118 10-4 T T (temperature in K and vapor pressure is in atmospheres). The critical temperature (Te) and critical pressure (Pc) of neopentane are 160.60°C and 31.57 atmospheres respectively. Using the information given above and the class notes, answer the questions #1. 1. The acentric factor w is used a characterization parameter in phase behavior calculations. Acentric factor is a measure of sphericity of a molecule. The definition of w is given below. psat @ =- log10 --1.0 prat is calculated at T/Tc= 0.7 Pc Here Pal is the vapor pressure of the component and, P. and T are critical properties of the component. Psat/P¢and T/Tc must be unitless (T and Tc must be in R or K). Calculate the acentric factor of neopentane (CSH12) using Antoine vapor pressure equation. (In data…arrow_forwardThe photons that make up the cosmic microwave background were emitted about 380,000 years after the Big Bang. Today, 13.8billion years after the Big Bang, the wavelengths of these photons have been stretched by a factor of about 1100 since they were emitted because lengths in the expanding universe have increased by that same factor of about 1100. Consider a cubical region of empty space in today’s universe 1.00 m on a side, with a volume of 1.00 m3. What was the length s0 of each side and the volume V0 of this same cubical region 380,000 years after the Big Bang? s0 = ? m V0 = ? m^3 Today the average density of ordinary matter in the universe is about 2.4×10−27 kg/m3. What was the average density ?(rho)0 of ordinary matter at the time that the photons in the cosmic microwave background radiation were emitted? (rho)0 = ? kg/m^3arrow_forwardA long-baseline neutrino diss-appearance experiment wants to measure neutrino oscillations with an expected squared mass difference of approximately Am² = 2.5x10-³ eV2. The neutrino beam energy is 3.7 GeV. Calculate the optimal distance between the near and the far detector in [km]. (Explain your solution in the worked script).arrow_forward
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