University Physics with Modern Physics (14th Edition)
14th Edition
ISBN: 9780321973610
Author: Hugh D. Young, Roger A. Freedman
Publisher: PEARSON
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 44, Problem 44.32E
To determine
The distance in light-years of this quasar from the earth.
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solution
Students have asked these similar questions
The rest wavelength of the Hα transition of atomic hydrogen is 656.3 nm (recall that 1 nm=10-9 m). If an observer takes a spectrum of a distant galaxy and identifies that line at 920 nm, what is the redshift of the galaxy? (recall that z=(λobs-λem)/λem ) If the value of the Hubble constant is Ho=71 km/s/Mpc, what is the approximate distance to the galaxy in Mpc?
Edwin Hubble observed that the light from very distant galaxies was redshifted and that the farther away a galaxy was, the greater its redshift. What does this say about very distant galaxies?
When Hubble first estimated the Hubble constant, galaxy distances were still very uncertain, and he got a value for H of about 600 km/s per Mpc. What would this have implied about the age of the universe?
What problems would this have presented for cosmologists?
The CaII H and K lines have rest wavelengths of 396.85 nm and 393.36 nm, respectively. In the spectrum of a galaxy in the cluster Abell 2065, the observed wavelengths of the two lines are 425.50 nm and 421.76 nm.
a) What is the redshift z of the galaxy?
b) What is the distance to the galaxy?
c) What is the distance modulus of the galaxy?
Chapter 44 Solutions
University Physics with Modern Physics (14th Edition)
Ch. 44.1 - Each of the following particles can be exchanged...Ch. 44.2 - Prob. 44.2TYUCh. 44.3 - From conservation of energy, a particle of mass m...Ch. 44.4 - Prob. 44.4TYUCh. 44.5 - Prob. 44.5TYUCh. 44.6 - Is it accurate to say that your body is made of...Ch. 44.7 - Prob. 44.7TYUCh. 44 - Prob. 44.1DQCh. 44 - Prob. 44.2DQCh. 44 - When they were first discovered during the 1930s...
Ch. 44 - The gravitational force between two electrons is...Ch. 44 - Prob. 44.5DQCh. 44 - Prob. 44.6DQCh. 44 - Prob. 44.7DQCh. 44 - Prob. 44.8DQCh. 44 - Prob. 44.9DQCh. 44 - Does the universe have a center? Explain.Ch. 44 - Prob. 44.11DQCh. 44 - Prob. 44.12DQCh. 44 - Prob. 44.13DQCh. 44 - Prob. 44.1ECh. 44 - Prob. 44.2ECh. 44 - Prob. 44.3ECh. 44 - Prob. 44.4ECh. 44 - Prob. 44.5ECh. 44 - Prob. 44.6ECh. 44 - Prob. 44.7ECh. 44 - An electron with a total energy of 30.0 GeV...Ch. 44 - Deuterons in a cyclotron travel in a circle with...Ch. 44 - The magnetic field in a cyclotron that accelerates...Ch. 44 - Prob. 44.11ECh. 44 - Prob. 44.12ECh. 44 - Prob. 44.13ECh. 44 - Prob. 44.14ECh. 44 - Prob. 44.15ECh. 44 - Prob. 44.16ECh. 44 - Prob. 44.17ECh. 44 - Prob. 44.18ECh. 44 - What is the mass (in kg) of the Z0? What is the...Ch. 44 - Prob. 44.20ECh. 44 - Prob. 44.21ECh. 44 - Prob. 44.22ECh. 44 - Prob. 44.23ECh. 44 - Prob. 44.24ECh. 44 - Prob. 44.25ECh. 44 - Prob. 44.26ECh. 44 - Prob. 44.27ECh. 44 - Prob. 44.28ECh. 44 - Prob. 44.29ECh. 44 - Prob. 44.30ECh. 44 - Prob. 44.31ECh. 44 - Prob. 44.32ECh. 44 - Prob. 44.33ECh. 44 - Prob. 44.34ECh. 44 - Prob. 44.35ECh. 44 - Prob. 44.36ECh. 44 - Prob. 44.37ECh. 44 - Prob. 44.38ECh. 44 - Prob. 44.39PCh. 44 - Prob. 44.40PCh. 44 - Prob. 44.41PCh. 44 - Prob. 44.42PCh. 44 - Prob. 44.43PCh. 44 - Prob. 44.44PCh. 44 - Prob. 44.45PCh. 44 - Prob. 44.46PCh. 44 - Prob. 44.47PCh. 44 - Prob. 44.48PCh. 44 - Prob. 44.49PCh. 44 - Prob. 44.50PCh. 44 - Prob. 44.51PCh. 44 - The K0 meson has rest energy 497.7 MeV. A K0 meson...Ch. 44 - DATA While tuning up a medical cyclotron for use...Ch. 44 - Prob. 44.54PCh. 44 - Prob. 44.55PCh. 44 - Consider a collision in which a stationary...Ch. 44 - Prob. 44.57PPCh. 44 - Prob. 44.58PPCh. 44 - Prob. 44.59PP
Knowledge Booster
Learn more about
Need a deep-dive on the concept behind this application? Look no further. Learn more about this topic, physics and related others by exploring similar questions and additional content below.Similar questions
- Most of the particles known to physicists are unstable. For example, the lifetime of the neutral pion,π0, is about 8.4x10-17 s. Its mass is 135.0 MeV/c2. a) What is the energy width of the π0 in its ground state? b) What is the relative uncertainty ∆m/m of the pion’s mass?arrow_forwardThe expanding universe is carrying distant objects away from each other at a rate proportional to their separations. We use the Doppler effect observed in spectra of distant galaxies and quasars to calculate recession speeds. For the most distant objects recession speeds approach c, and therefore, the relativistic Doppler shift expression must be used. We define the redshift, z, as the fractional change in wavelength. a) The most distant quasar currently known is ULAS J1120+0641, discovered with the UK Infrared Telescope on Mauna Kea. It has a redshift of 7.1. Calculate its radial velocity in terms of v/c. b) Determine the distance to this quasar. c) At what wavelength would the Ha line (656.28 nm) be observed for this quasar?arrow_forwardIn vacuum, the H-alpha line has a rest-frame wavelength of 656.461 nm. You took a spectrum of the center of a galaxy at an observatory on the ground and measured a wavelength of 656.65 nm for the H-alpha line. What is the radial velocity of the galaxy relative to the observer [km/s]? Note that the index of refraction of air is 1.0003 at that wavelength. As a result, the rest-frame wavelength of the H-alpha line in air differs from the rest-frame wavelength in vacuum.arrow_forward
- The gravitational wave source GW 170817 was used to obtain an estimate of the Hubble Constant of Ho = 72 ± 10 km s¹ Mpc-¹. How many other similar GW sources need to be observed if we want to reduce the standard error on Ho to less than 3%?arrow_forwardA galaxy has a redshift of z = = 0.15 and you are asked to determine the wavelengths at which its Call H and K lines would appear in the observed spectrum. The rest-frame wavelengths of the Call H and K lines are o 3968.5 Å and 3933.6 Å, respectively. NOTE: assume H₁ = 72 kms¯¹ Mpc¯¹. = (a) Calculate the observed wavelengths for the Call H and K lines. (b) What is the velocity of recession for this galaxy and it's distance in Mpc?arrow_forwardThe bright radio galaxy, 3c84, is observed to be moving away from the Earth at such high speed that the emitted blue 434-nm Hγ line of hydrogen is Doppler-shifted to 442 nm. Edwin Hubble discovered that all objects outside the local group of galaxies are moving away from us, with speeds v proportional to their distances R. Hubble's law is expressed as v = HR, where the Hubble constant has the approximate value H ≈ 22 ✕ 10−3 m/(s · ly). Determine the distance from the Earth to this galaxy. _________ lyarrow_forward
- The peak intensity of the CMBR occurs at a wavelength of 1.1 mm. (a) What is the energy in eV of a 1.1-mm photon? (b) There are approximately 109 photons for each massive particle in deep space. Calculate the energy of 109 such photons. (c) If the average massive particle in space has a mass half that of a proton, what energy would be created byconverting its mass to energy? (d) Does this imply that space is “matter dominated”? Explain briefly.arrow_forwardA galaxy in the constellation Pisces is 5210 Mly from the earth. (a) Use the Hubble law to calculate the speed at which this galaxy is receding from earth. (b) What redshifted ratio l0 /lS is expected for light from this galaxy?arrow_forwarda)Define the term “standard candle” as used in cosmology. b)The flux is defined asf(Dlum) = L/4πD^2lumwhere L is the absolute luminosity and Dlum is the distance to the radiation source (youmay assume z ≪ 1).Assume that we have measured the flux to be f = 7.234 10^−23 Wm^−2 and the absoluteluminosity is given by L = 3.828 x10^26W. Calculate the luminosity distance D lum to the objectin Mpc.arrow_forward
- P2 X The image to the left is a Feynman diagram with time increasing upward. P1 (a) If p1 is an electron and X is a W+ what must p2 be? Why? (b) If p1 is a μ+ and p2 is a different flavor of lepton, what must p2 be? Why? (c) In the last question, what must X be? Why? (d) If p1 and p2 are both electron neutrinos, what must X be? Why? (e) If p1 and p2 are both the same flavor of charged lepton, what might X be? (There are two possibilities.) Why?arrow_forwardIn the Check Your Learning section of Example 27.1, you were told that several lines of hydrogen absorption in the visible spectrum have rest wavelengths of 410 nm, 434 nm, 486 nm, and 656 nm. In a spectrum of a distant galaxy, these same lines are observed to have wavelengths of 492 nm, 521 nm, 583 nm, and 787 nm, respectively. The example demonstrated that z=0.20 for the 410 nm line. Show that you will obtain the same redshift regardless of which absorption line you measure.arrow_forwardConsider the energy-momentum tensorT_µν = (ρ + p) u_µ u_ν + p g_µνapplied to the matter/energy distribution in the universe on large scales, and assume an equation of state of the form p = wρ, with w a constant. Determine the type of matter/energy dominating the universe if the energy-momentum tensor is traceless, that is, T^µ_µ = 0.arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
Principles of Physics: A Calculus-Based TextPhysicsISBN:9781133104261Author:Raymond A. Serway, John W. JewettPublisher:Cengage Learning
Physics for Scientists and Engineers with Modern ...PhysicsISBN:9781337553292Author:Raymond A. Serway, John W. JewettPublisher:Cengage Learning
Modern PhysicsPhysicsISBN:9781111794378Author:Raymond A. Serway, Clement J. Moses, Curt A. MoyerPublisher:Cengage Learning
AstronomyPhysicsISBN:9781938168284Author:Andrew Fraknoi; David Morrison; Sidney C. WolffPublisher:OpenStax
Principles of Physics: A Calculus-Based Text
Physics
ISBN:9781133104261
Author:Raymond A. Serway, John W. Jewett
Publisher:Cengage Learning
Physics for Scientists and Engineers with Modern ...
Physics
ISBN:9781337553292
Author:Raymond A. Serway, John W. Jewett
Publisher:Cengage Learning
Modern Physics
Physics
ISBN:9781111794378
Author:Raymond A. Serway, Clement J. Moses, Curt A. Moyer
Publisher:Cengage Learning
Astronomy
Physics
ISBN:9781938168284
Author:Andrew Fraknoi; David Morrison; Sidney C. Wolff
Publisher:OpenStax