Essential University Physics (3rd Edition)
3rd Edition
ISBN: 9780134202709
Author: Richard Wolfson
Publisher: PEARSON
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Chapter 39, Problem 37E
To determine
Using the Hubble constant
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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%?
I have tried 14,000,000,000, 17,908,900,000, and 17.9089 x 10^9 for the hubble time and all those are wrong. I have tried 17,908,900,000 and 17.9089 x 10^9 for the second question and those are wrong too. There are two parts to this questions. Thank you!
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?
Chapter 39 Solutions
Essential University Physics (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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- a) Define the term “standard candle” as used in cosmology b). The flux is defined as f(Dlum) = L /4πD2lum , where L is the absolute luminosity and Dlum is the distance to the radiation source (you may assume z ≪ 1). Assume that we have measured the flux to be f = 7.234 10−23Wm−2 and the absolute luminosity is given by L = 3.828 1026W. Calculate the luminosity distance Dlum to the object in Mpc. c). Calculate the distance modulus µ for the object of the previous subquestion. Show that the distance modulus µ can be written as given in imagearrow_forwardSuppose the energy density of the cosmological constant is equal to the present critical density En = Ec.0 = 4870MeVm-3. What is the total energy of the cosmological constant within a sphere 1AU in radius?What is the rest energy of the Sun (Eo = Moc²)? Comparing these two numbers, do you expect the cosmological constant to have a significant effect on the motion of planets within the solar system?arrow_forwardc. The critical density for the Universe is given by 3H% Pcrit 8TG Calculate the ratio between the values derived for the critical density of the Universe assuming Ho = H5 Planck and Ho = H° = HSHOESarrow_forward
- a)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_forwardThe 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?arrow_forwardThere are two parts to this question. I need to know the years for both. I have tried 14,000,000,000, 17,908,900,000, 17.29 x 10^9, and 17.9089 x 10^9 for the hubble time and all those are wrong. I have tried 17,908,900,000, 17.29 x 10^9, and 17.9089 x 10^9 for the second question and those are wrong too.arrow_forward
- The mass of the neutrino plays an important role in the universe. Suppose the mass of two neutrinos in the universe is 4.8×10-³5 kg and the current Hubble’s constant is 72 km/s/Mpc. The critical density of the universe is five times the average density of the universe. Estimate the number of neutrons present per cubic meter in the universe. (a) 2.1×10⁹ (b) 4.1×10² (c) 1.1x10° (d) 8.1×107arrow_forwardConsider a universe where Big Bang nucleosynthesis produced significantly more 4He than 1H. Estimate the observed redshift, z, of the Cosmic Radiation Background (CMB) by an observer that observes the CMB to have a blackbody temperature of 2.715 K. Assume this universe has Ob = 0. 0486, QDM = O. 2588 and QA = 0. 6911arrow_forwardEdwin 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?arrow_forward
- If the average density of the Universe is small compared with the critical density, the expansion of the Universe described by Hubble's law proceeds with speeds that are nearly constant over time. Calculate t since the big bang, assuming H = 22.0 km/s/Mly.arrow_forwardUse Wien’s law to answer the following questions: (a) The cosmic background radiation peaks in intensity at a wavelength of 1.1 mm. To what temperature does this correspond? (b) About 379 000 y after the big bang, the universe became transparent to electromagnetic radiation. Its temperature then was 2970 K.What was the wavelength at which the background radiation was then most intense?arrow_forwardName: Hubble Distances Redshift z parameter The relativistic redshift is parametrized by z and given by Δ In terms of the scale factor, 2= X do - de de 1+z= ao a (2) Problem 01. Find the redshift z for a Hydrogen spectral line originally at 656 nm which has been observed at a wavelength of 1.64 μm. Astro 001 Fall 2022 Problem 02. How much smaller was the universe when this light was emitted? U₁ = DHO Using the redshift to measure the velocity, we find D~ (1) 0.1 Hubble's Law Hubble's Law states that the recession velocity of a redshifted galaxy is given by the product of the distance and the Hubble constant. (3) ZC Ho where c = 3 x 108 m/s and Ho = 2.3 x 10-18 s in standard units. The standard measurement of the Hubble constant is Ho = 71 (km/s)/Mpc. Problem 03. What is the distance in Mpc and ly to the galaxy measured in problem 01? 1 pc = 3.26 ly.arrow_forward
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