Ex. 74 Calculate the energy radiated in one had of minute by a black body of surface area 400 cm² when it is maintained at 127°C. (Stefan's constant o = 5.7 x 10-8 S. I. units)
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- 2.9. (a) Solve the integral ...| (dx .dx3N) 3N and use it to determine the "volume" the relevant region of the phase space of an extreme relativistic gas ( = pc) of 3N particles moving in one dimension. Determine, as well, the number of ways of distributing a given energy E among this system of particles and show that, asymptotically, w0 = h³N. (b) Compare the thermodynamics of this system with that of the system considered in Problem 2.8.P X %23 in a 20 poster wal Sp Sp famu.instructure.com/courses/9823/assignments/177283 M Update : THERMAL RADIATION 2 FLORIDA MECHANICAL AGRICULTURA HEAD HEART HAND Problem 4. Planetary Temperatures: Radiation of Heat to Space (Palen, et. al. 1st Ed. Chapter 6 Problem 63 ) FIELD Working It Out 6.2 The Stefan-Boltzmann Law Account Look at Figure 6.17, which shows the spectra of a light source at several different temperatures. This source is assumed to emit electromagnetic radiation only because of its temperature, not its composition. This kind of source is called a blackbody, and if we graph the intensity of its emitted radiation across all wave- lengths (as in Figure 6.17), we obtain a characteristic curve called a blackbody spectrum. As the object's temperature increases, it emits more radiation at every wavelength, so each increase in temperature raises the curve. The luminosity of the object (the total amount of light emitted) increases. In fact, it increases quite fast as the…In this problem you will consider the balance of thermal energy radiated and absorbed by a person. Assume that the person is wearing only a skimpy bathing suit of negligible area. As a rough approximation, the area of a human body may be considered to be that of the sides of a cylinder of length L=2.0m and circumference C=0.8m. For the Stefan-Boltzmann constant use ?=5.67
- 4. Derive the maxwell equations for U, H, G and A Table 6.2.1: Maxwell Relations Function U H A G Differential dU = TdS-pdV dH = TdS + Vdp dA=-pdV - SdT dG = Vdp - SdT Natural Variables S, V S, P V, T P, T Maxwell Relation (or)--( др as V (37), = (35), as (OP), - (OV), = V (3r), - - (35), = Tno handwrittenFind a formula for the temperature of an Einstein solid in the limit q « N . Solve for the energy as a function of temperature to obtain U = N€e-€/kT (where € is the size of an energy unit).
- Two stars, both of which behave like ideal blackbodies, radiate the same total energy per second. The cooler one has a surface temperature T and 4.0 times the diameter of the hotter star. What is the temperature of the hotter star in terms of T? (Just write the result)The Earth reradiates the energy it receives from the Sun as a black body. We can calculate the effective temperature of the Earth using the Stefan-Boltzmann equation F = sT4 where we solve for the Temperature T. We use for the energy flux the amount of energy absorbed per second Le divided by the Earth's surface area from which the energy is radiated 4pd2 so that the flux is = Le/(4pd2). Here d is the radius of the Earth given above and s is the Stefan-Boltzmann constant. And the effective temperature is:Te4 = (Le/(4pd2))/s = Le/(4spd2) = __________________ K4and taking the square root of Te4 twice in succession we get the effective Temperature Te:Te = [Le/(4spd2)]0.25 = _________________ Kfor the temperature of the effective Earth. What is the temperature in the Celsius scale? __________ C. (Do I need to tell you how to convert from Kelvin to Celsius? If you don't know look it up in your textbook!!)