/*! This file is auto-generated */ .wp-block-button__link{color:#fff;background-color:#32373c;border-radius:9999px;box-shadow:none;text-decoration:none;padding:calc(.667em + 2px) calc(1.333em + 2px);font-size:1.125em}.wp-block-file__button{background:#32373c;color:#fff;text-decoration:none} Q. 7.52 (a) Estimate (roughly) the total... [FREE SOLUTION] | 91Ó°ÊÓ

91Ó°ÊÓ

(a) Estimate (roughly) the total power radiated by your body, neglecting any energy that is returned by your clothes and environment. (Whatever the color of your skin, its emissivity at infrared wavelengths is quite close to 1; almost any nonmetal is a near-perfect blackbody at these wavelengths.)

(b) Compare the total energy radiated by your body in one day (expressed in kilocalories) to the energy in the food you cat. Why is there such a large discrepancy?

(c) The sun has a mass of 2×1030kgand radiates energy at a rate of 3.9×1026watts. Which puts out more power per units mass-the sun or your body?

Short Answer

Expert verified

(a) . The total power radiated by our body 1kW

(b) .role="math" localid="1647768533942" The energy we would lose in one dayis20,000cal.

(c) .The radiation rate per kilogramis0.0002W/kg

Step by step solution

01

Step 1. Given information

  • The total power radiated by our body we use is given by Power=σeAT4
02

Step 2. Calculating the total power radiated by our body we use .

The power radiated is

Power=σeAT4

T=310K, A=2m2, e=1.

Power=5.67×10-8W/m2·K42m2(310K)4

=1050W

≈1000W

≈1.0×103W

≈1kW

Hence, This is the rate at which we would lose energy, if we were naked in empty space .

03

Step 3. Calculating the energy we would lose in one day .

The rate, the energy we would lose in one day will be

(1050W)(24hr)3600s1hr=9.0×107J1kcal4186J

=20,000kcal

As we can see that it is ten times the numbers of calories that an average person conserves in a day about (2000). The discrepancy is due to the fact that we are not naked in empty space, most of the energy that we radiate is replaced by energy radiated or conducted back to us by our clothes and other surroundings

04

Step 4. Calculating the radiation rate per kilogram.

Now, the radiation rate per kilogram is

1000W75kg=14W/kgin case of seen it is

3.9×1026W2×1030kg=0.0002W/kg

As it is 70,000 times less, have we get a reason that, how is it possible of although the sun is bright it is also very massive. Although it generates energy by nuclear fusion the reaction in its core actually proceeds extremely slowly giving it a ten billion year life time. So, I on the other hand have to replenish my chemical fuel supply on daily basis.

Unlock Step-by-Step Solutions & Ace Your Exams!

  • Full Textbook Solutions

    Get detailed explanations and key concepts

  • Unlimited Al creation

    Al flashcards, explanations, exams and more...

  • Ads-free access

    To over 500 millions flashcards

  • Money-back guarantee

    We refund you if you fail your exam.

Over 30 million students worldwide already upgrade their learning with 91Ó°ÊÓ!

One App. One Place for Learning.

All the tools & learning materials you need for study success - in one app.

Get started for free

Most popular questions from this chapter

Carry out the Sommerfeld expansion for the energy integral (7.54), to obtain equation 7.67. Then plug in the expansion for μto obtain the final answer, equation 7.68.

For a system of bosons at room temperature, compute the average occupancy of a single-particle state and the probability of the state containing 0,1,2,3bosons, if the energy of the state is

(a) 0.001eVgreater than μ

(b) 0.01eVgreater than μ

(c) 0.1eVgreater than μ

(d) 1eVgreater than μ

Sometimes it is useful to know the free energy of a photon gas.

(a) Calculate the (Helmholtz) free energy directly from the definition

(Express the answer in terms of T' and V.)

(b) Check the formula S=-(∂F/∂T)Vfor this system.

(c) Differentiate F with respect to V to obtain the pressure of a photon gas. Check that your result agrees with that of the previous problem.

(d) A more interesting way to calculate F is to apply the formula F=-kTlnZ separately to each mode (that is, each effective oscillator), then sum over all modes. Carry out this calculation, to obtain

F=8πV(kT)4(hc)3∫0∞x2ln1-e-xdx

Integrate by parts, and check that your answer agrees with part (a).

For a brief time in the early universe, the temperature was hot enough to produce large numbers of electron-positron pairs. These pairs then constituted a third type of "background radiation," in addition to the photons and neutrinos (see Figure 7.21). Like neutrinos, electrons and positrons are fermions. Unlike neutrinos, electrons and positrons are known to be massive (ea.ch with the same mass), and each has two independent polarization states. During the time period of interest, the densities of electrons and positrons were approximately equal, so it is a good approximation to set the chemical potentials equal to zero as in Figure 7.21. When the temperature was greater than the electron mass times c2k, the universe was filled with three types of radiation: electrons and positrons (solid arrows); neutrinos (dashed); and photons (wavy). Bathed in this radiation were a few protons and neutrons, roughly one for every billion radiation particles. the previous problem. Recall from special relativity that the energy of a massive particle is ϵ=(pc)2+mc22.

(a) Show that the energy density of electrons and positrons at temperature Tis given by

u(T)=∫0∞x2x2+mc2/kT2ex2+mc2/kT2+1dx;whereu(T)=∫0∞x2x2+mc2/kT2ex2+mc2/kT2+1dx

(b) Show that u(T)goes to zero when kT≪mc2, and explain why this is a

reasonable result.

( c) Evaluate u(T)in the limit kT≫mc2, and compare to the result of the

the previous problem for the neutrino radiation.

(d) Use a computer to calculate and plot u(T)at intermediate temperatures.

(e) Use the method of Problem 7.46, part (d), to show that the free energy

density of the electron-positron radiation is

FV=-16π(kT)4(hc)3f(T);wheref(T)=∫0∞x2ln1+e-x2+mc2/kT2dx

Evaluate f(T)in both limits, and use a computer to calculate and plot f(T)at intermediate

temperatures.

(f) Write the entropy of the electron-positron radiation in terms of the functions

uTand f(T). Evaluate the entropy explicitly in the high-T limit.

Consider a Bose gas confined in an isotropic harmonic trap, as in the previous problem. For this system, because the energy level structure is much simpler than that of a three-dimensional box, it is feasible to carry out the sum in equation 7.121 numerically, without approximating it as an integral.*

(a) Write equation 7.121 for this system as a sum over energy levels, taking degeneracy into account. Replace Tandμwith the dimensionless variables t=kT/hfandc=μ/hf.

(b) Program a computer to calculate this sum for any given values of tandc. Show that, for N=2000, equation 7.121 is satisfied at t=15provided that c=-10.534. (Hint: You'll need to include approximately the first 200 energy levels in the sum.)

(c) For the same parameters as in part (b), plot the number of particles in each energy level as a function of energy.

(d) Now reduce tto 14 , and adjust the value of cuntil the sum again equals 2000. Plot the number of particles as a function of energy.

(e) Repeat part (d) for t=13,12,11,and10. You should find that the required value of cincreases toward zero but never quite reaches it. Discuss the results in some detail.

See all solutions

Recommended explanations on Physics Textbooks

View all explanations

What do you think about this solution?

We value your feedback to improve our textbook solutions.

Study anywhere. Anytime. Across all devices.