Use the Planck distribution law(7.28) to calculate the total energy density of a black-body at a temperature of 3000K.
Use the Planck distribution law(7.28) to calculate the total energy density of a black-body at a...
Derive the long wavelength limit of the Planck energy density distribution.
Derive the long wavelength limit of the Planck energy density distribution
The energy radiated per unit surface area (across all wavelengths) for a black body with temperature 2200. Use 5.67 x 10-8 for the Stefan-Boltzmann constant. The Stefan-Boltzmann Law describes the power radiated from a black body in terms of its temperature. Specifically, the total energy radiated per unit surface area of a black body across all wavelengths per unit time is proportional to the fourth power of the black body's thermodynamic temperature
A black body has an effective surface temperature of 450°C. Determine: (a) The total radiation energy (W/m2) that can be emitted by the black body (b) Determine total radiation energy (W/m%) that can be emitted by the black body within the 5-50 um wavelength region (c) The spectral blackbody emissive power of the black body at a wavelength of 10 um. 12
(a) Calculate the sun’s energy output assuming the sun is a black body radiator at 5800K surface temperature, and its diameter is 1.39E+06 km. (b) (And) from the earth orbit diameter calculate the energy actually reaching the top of the earth’s atmosphere, and compare it to the solar constant.
8. A black body has an effective surface temperature of 450°C. Determine: (a) The total radiation energy (W/m²) that can be emitted by the black body (b) Determine total radiation energy (W/m²) that can be emitted by the black body within the 5-50 um wavelength region (c) The spectral blackbody emissive power of the black body at a wavelength of 10 um.
Properties of a truncated sphere with a power law density profile Suppose the mass distribution of an elliptical galaxy is spherically symmetric, and its density profile is given by ρ(r)=po(r/rs)-2 a(r) =0 for for r<r, r>rs The important difference compared to the 3D→2D projection problem we considered in class is that this 3D density profile does not extend to infinity, but is truncated at r = rs. (a) Calculate the projected half mass-radius, Re of this mass distribution. First, you...
1. The solar energy spectral density is shown in the right figure. By assuming that the sun is a blackbody, use the Planck's distribution function to fit the extraterrestrial solar energy spectral density. Extraterrestrial (a) Determine the most possible surface temperature T of sun by fitting the Planck's distribution to the extraterrestrial solar energy spectral density. You can choose a few temperatures to see which temperature can best fit the peak (at Amsx) and the entire profile of the extraterrestrial...
u(λ,T)=4E(λ,T)/c
2. Use the energy density expression above and the Stefan-Boltzmann expression, u(T) 014 with σ= 7.56x 10.15 erg/cmK4, to obtain a formula for the total rate of radiation per unit area of a black body. Assume that the sun radiates as a black body. You are given the radius of the sun R -7x101° cm, the average distance of the sun to the earth d Lx10 c, nthe solar consdant, the aount of enexgy : carth when the sun...
(i) A total radiation thermometer (calibrated with a black body) reads a brightness temperature of 427 degrees celcius on a section of an opaque reactor wall which has a total grey emissivity, of 0.8. Write the formula allowing the determination of its true temperature, Tt1, and calculate Tt1 to the nearest degree °C. Determine the relative error (in %) made when neglecting the emissivity correction.