Essential University Physics: Volume 2 (3rd Edition)
3rd Edition
ISBN: 9780321976420
Author: Richard Wolfson
Publisher: PEARSON
expand_more
expand_more
format_list_bulleted
Concept explainers
Question
Chapter 39, Problem 49P
To determine
The diameter of the sun to have expanded to get average density
8.65 × 10 − 27 kg ⋅ m -3
Expert Solution & Answer
Want to see the full answer?
Check out a sample textbook solutionStudents have asked these similar questions
what is the rate that sun loose energy by radiation?Given the sun temperature is about 6000k and its radius is 6.95x10^5 kms ( answer shouild be in watts)
In the Sun's core, thermonuclear reactions produce the energy which
2.
eventually produces the Sun's luminosity. The Sun's core has a temperature,
Tcore 1.6 x 107 K. The mass density of the core is approximately p= 1.5
x 10 kg m3. Assuming the core has the same mass fraction of hydrogen
as the Sun's atmosphere (XH = 0.75), approximate the number of fusion
reactions between two hydrogen nuclei (two free protons) per second. You
may assume that the temperature and density are uniform throughout the
core (not realistic!), which extends from the center of the sun out to about
Ro/5, and that particles within the core act like a non-relativistic ideal gas
(Maxwellian velocity distribution) with all reactions happening at the same
relative velocity. Also assume the cross-sectional area for a proton-proton
reaction is o = 2.75 x 1048 m2.
%3D
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…
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
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
- (a) Estimate the mass of the luminous matter in the known universe, given there are 1011 galaxies, each containing 1011 stars of average mass 1.5 times that of our Sun. (b) How many protons (the most abundant nuclide) are there in this mates? (c) Estimate the total number of particles in the observable universe by multiplying the answer to (b) by two, since there is an electron for each proton, and then by 109, since there are far more particles (such as photons and neutrinos) in space than in luminous matter.arrow_forwardDerive the relationship between root mean square velocity and most probable velocity. The root mean square velocity of hydrogen is 21 × 105 cm sec–1. Calculate its most probable velocity in cm sec-1arrow_forward39. An isotropic point source emitting S, neutrons/s is placed in the center of a bare sphere of radius R. The sphere is made up of carbon (L = D/E.). Show that the general solution for flux inside the sphere is given by: Ø(r) = Le-rl +으 r r where C and C2 are constants of integration. Apply the boundary conditions and find the neutron flux anywhere at r = R/2. [Hint: Start with Equation VIe.2.14 and make a change of function; ø = plr]. 2R Point Source Problem 39 Problem 40 Problem 41 1 d dø(r)]_ E. s(r) -$(r) = D VIe.2.14 p2 dr dr 40. Solve problem 39 considering the sphere is located in an infinite medium made up of water. made up of water. .--- 8arrow_forward
- 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_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_forwardEx. 84: Taking collar constant as 1340 watt/m² minute. Calculate black body temperature per of the sun, from following data. o = 5.67 x 10-* W/ m² K¹, Radius of sun R = 7 x 10 km. The distance between sun and earth = 1.496 x 10³ kmarrow_forward
- You are performing work as an assistant to a cosmology professor. She asks you to estimate the temperature of the Universe at a time after the Big Bang when neutral atoms could form from the plasma and the Universe became transparent. She tells you that the energy required to excite an atom is on the order of 1 eV. She suggests you use the Boltzmann distribution function e-E/k BT to find the order of magnitude of the threshold temperature at which 1.00% of a population of photons has energy greater than 1.00 eV.arrow_forwardDetermine the Debye length in meter if the plasma temperature is 2 eV and the plasma density is 5*10^24 cm-3 ?arrow_forwardWe 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:…arrow_forward
- Midterm G Which of the following cc locs.google.com/forms/d/e/1FAlpQLSehenyKBfzpwA6Ba1LyJILHfOLpHNWF menian America... yyyyyyyyyu E Untitled document -. Alpha particles are electrons helium nuclei negative neutral When an elecuon movesarrow_forwardassume you are a perfect black body and Temp=310K. At what rate, in watts, do you radiated energy? (assume that you are spherical and have the density of water)arrow_forwardIn a controlled fusion reactor Deuterium-Tritium The temperature of the plasma is T = 10 keV, where k is the k Boltzmann constant. The ions' number density is 2.6×10¹8 m-3. -22 3 Moreover (ov) = 10-²²m³s-¹, where o is the reaction cross-section, v is the relative speed of the reacting particles, and represents averaging according to the Maxwell- Boltzmann distribution. fusion is occurring. For what value of the confinement time does the reactor achieve the break even point? Enter your answer in seconds to 1 decimal point.arrow_forward
arrow_back_ios
SEE MORE QUESTIONS
arrow_forward_ios
Recommended textbooks for you
- Modern PhysicsPhysicsISBN:9781111794378Author:Raymond A. Serway, Clement J. Moses, Curt A. MoyerPublisher:Cengage LearningCollege PhysicsPhysicsISBN:9781938168000Author:Paul Peter Urone, Roger HinrichsPublisher:OpenStax College
Modern Physics
Physics
ISBN:9781111794378
Author:Raymond A. Serway, Clement J. Moses, Curt A. Moyer
Publisher:Cengage Learning
College Physics
Physics
ISBN:9781938168000
Author:Paul Peter Urone, Roger Hinrichs
Publisher:OpenStax College