Essentials University Physics, Volume 1 and 2 - With Modified MasteringPhysics Access
3rd Edition
ISBN: 9780134235448
Author: Wolfson
Publisher: PEARSON
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Question
Chapter 39, Problem 54P
(a)
To determine
The median wavelength of the newly formed cosmic microwave background
(b)
To determine
The photon energy of cosmic microwave background radiation when the universe was formed.
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Chapter 39 Solutions
Essentials University Physics, Volume 1 and 2 - With Modified MasteringPhysics Access
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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- Because of the cosmological expansion, a particular emission from a distant galaxy has a wavelength that is 2.00 times the wavelength that emission would have in a laboratory. Assuming that Hubble’s law holds and that we can apply Doppler-shift calculations, what was the distance (ly) to that galaxy when the light was emitted?arrow_forwardWhat effect does increasing the interaction strength of a massive particle species haveon its thermal relic abundance if it was in thermal equilibrium in the early universe(assuming no initial asymmetry)? a. relic abundance increases b. relic abundance decreases c. relic abundance essentially unchanged d. not enough informationarrow_forwardSuppose the Universe is dominated by a strange substance with an equation of state w = -0.7. This substance fills the Universe in a uniform way, and is the only dynamically important constituent. Suppose further that in some time interval the Universe doubles in (linear) size, i.e. the scale factor doubles. By what factor has the energy density of this substance changed during this time interval, i.e., what is εfinal/εinitial? The energy density substance dilutes in proportion to a to some power p, i.e. ε(a) ∝ aparrow_forward
- If the mass-density of baryonic matter is rhoM = 10^-28 kg m^-3 and the current temperature of the cosmic microwave background is T = 2.7 K, calculate: (a) The mass-density of radiation (i.e rhoR) (b) The photon-baryon ratio (c) The temperature when rhoR = rhoMarrow_forwardClassical general relativity views the structure of spacetime as deterministic and well defined down to arbitrarily small distances. On the other hand, quantum general relativity forbids distances smaller than the Planck length given by L = (hG/c3)1/2. (a) Calculate the value of the Planck length. The quantum limitation suggests that after the Big Bang, when all the presently observable section of the Universe was contained within a point-like singularity, nothing could be observed until that singularity grew larger than the Planck length. Because the size of the singularity grew at the speed of light, we can infer that no observations were possible during the time interval required for light to travel the Planck length. (b) Calculate this time interval, known as the Planck time T, and state how it compares with the ultrahot epoch mentioned in the text.arrow_forwardWhich particles are not present in the universe at t=300s after the big bang ? select one : a. Electons b. photons c. neutrons d. Positronsarrow_forward
- The temperature of the universe is 2.76 K. What is the wavelength of the cosmic background radiation, in millimeters?arrow_forwardThe Klein-Gordon equation at background level for a scalar field φ is given by (found in image below) where H is the Hubble parameter, V the potential of the scalar field, and V′ = dV/dφ.Assume a flat Friedmann-Robertson-Walker universe, dominated by the scalar field.i) State the conditions for slow-roll inflation. Write down the Friedmann equation and theKlein-Gordon equation valid for slow-roll inflation.ii) For a scalar field potential V =1/2m^2φ^2, where m is the mass of the field, calculate thetime evolution of the field φ in the case of slow-roll inflation.arrow_forward
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