Physics, 31.08.2019 02:10, Serenitybella

Calculate the intensity of thermal radiation from a blackbody by using raleigh-jeans law at a temperature of 1000 k and with a wavelength of 1000 nm (infrared), 500 nm (visible), and 100 nm (ultraviolet). (3 points) (b) recalculate the above intensities using plank's law

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answered: milagritomiracle

Explanation:

Given that,

Temperature = 1000 K

We need to calculate the intensity of thermal radiation from a black body

For wavelength 1000 nm

Using Raleigh-Jeans Law

$B_{k}=\dfrac{8\pi kT}{\lambda^4}$

Put the value into the formula

$B_{k}=\dfrac{8\times\pi\times1.38\times10^{-23}\times1000}{(1000\times10^{-9})^{4}}$

$B_{k}=346831.828956$

$B_{k}=34.68\times10^{4}\ W$

For wavelength 500 nm

$B_{k}=\dfrac{8\times\pi\times1.38\times10^{-23}\times1000}{(500\times10^{-9})^{4}}$

$B_{k}=5549309$

$B_{k}=55.49\times10^{5}\ W$

For wavelength 100 nm

$B_{k}=\dfrac{8\times\pi\times1.38\times10^{-23}\times1000}{(100\times10^{-9})^{4}}$

$B_{k}=3.47\times10^{9}\ W$

We need to calculate the intensity

Using Plank's Law

$E=\dfrac{2hc^2}{\lambda^5}\times\dfrac{1}{e^{\dfrac{hc}{\lambda k T}}-1}$

For wavelength 1000 nm

Put the value into the formula

$E=\dfrac{2\times6.63\times10^{-34}\times(3\times10^{8})^2}{(1000\times10^{-9})^5}\times\dfrac{1}{e^{\dfrac{6.63\times10^{-34}\times3\times10^{8}}{1000\times10^{-9}\times 1.38\times10^{-23}\times1000}}-1}$

$E=65.65\times10^{6}\ W/m^2.K^4$

For wavelength 500 nm

$E=\dfrac{2\times6.63\times10^{-34}\times(3\times10^{8})^2}{(500\times10^{-9})^5}\times\dfrac{1}{e^{\dfrac{6.63\times10^{-34}\times3\times10^{8}}{500\times10^{-9}\times 1.38\times10^{-23}\times1000}}-1}$

$E=11.56\times10^{2}\ W/m^2.K^4$

For wavelength 100 nm

$E=\dfrac{2\times6.63\times10^{-34}\times(3\times10^{8})^2}{(100\times10^{-9})^5}\times\dfrac{1}{e^{\dfrac{6.63\times10^{-34}\times3\times10^{8}}{100\times10^{-9}\times 1.38\times10^{-23}\times1000}}-1}$

$E=3.032\times10^{-44}\ W/m^2.K^4$

Hence, This is the required solution.

answered: Guest

sequence is a continuous and distinctive band of stars that appears on plots of stellar color versus brightness. these color-magnitude plots are known as hertzsprung–russell diagramsafter their co-developers, ejnar hertzsprungand henry norris russell. stars on this band are known as main-sequence stars or dwarf stars. these are the most numerous true stars in the universe, and include the earth's sun.after condensation and ignition of a star, it generates thermal energy in its dense core region through nuclear fusion of hydrogen into helium. during this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass, but also based upon its chemical composition and age. the cores of main-sequence stars are in hydrostatic equilibrium, where outward thermal pressure from the hot core is balanced by the inward pressure of gravitational collapse from the overlying layers. the strong dependence of the rate of energy generation on temperature and pressure to sustain this balance. energy generated at the core makes its way to the surface and is radiated away at the photosphere. the energy is carried by either radiation or convection, with the latter occurring in regions with steeper temperature gradients, higher opacity or both.the main sequence is sometimes divided into upper and lower parts, based on the dominant process that a star uses to generate energy. stars below about 1.5 times the mass of the sun (1.5 m☉) primarily fuse hydrogen atoms together in a series of stages to form helium, a sequence called the proton–proton chain. above this mass, in the upper main sequence, the nuclear fusion process mainly uses atoms of carbon, nitrogen and oxygen as intermediaries in the cno cycle that produces helium from hydrogen atoms. main-sequence stars with more than two solar masses undergo convection in their core regions, which acts to stir up the newly created helium and maintain the proportion of fuel needed for fusion to occur. below this mass, stars have cores that are entirely radiative with convective zones near the surface. with decreasing stellar mass, the proportion of the star forming a convective envelope steadily increases. main-sequence stars below 0.4 m☉undergo convection throughout their mass. when core convection does not occur, a helium-rich core develops surrounded by an outer layer of hydrogen.in general, the more massive a star is, the shorter its lifespan on the main sequence. after the hydrogen fuel at the core has been consumed, the star evolves away from the main sequence on the hr diagram, into a supergiant, red giant, or directly to a white dwarf.

answered: Guest

It may possibly be c i think |-/