If the human body is well approximated by a black body with tem- perature T = 310◦ K (98.6◦ F). At what wavelength (λ) do we emit the most energy (λmax)? How much energy per area (flux) do we emit? Remember the value of the Stefan-Boltzmann constant is σ = 5.67 × 10−5erg/(cm2K4s1). What kind of radiation (region of the electromagnetic spectrum) do we emit most of?

If the human body is well approximated by a black body with tem- perature T = 310◦ K (98.6◦ F). At what wavelength (λ) do we emit the most energy (λmax)? How much energy per area (flux) do we emit? Remember the value of the Stefan-Boltzmann constant is σ = 5.67 × 10−5erg/(cm2K4s1). What kind of radiation (region of the electromagnetic spectrum) do we emit most of?

Modern Physics

3rd Edition

ISBN:9781111794378

Author:Raymond A. Serway, Clement J. Moses, Curt A. Moyer

Publisher:Raymond A. Serway, Clement J. Moses, Curt A. Moyer

Chapter16: Cosmology

Section: Chapter Questions

Problem 10P

See similar textbooks

Similar questions

Suppose a star with radius 8.51 108 m has a peak wavelength of 689 nm in the spectrum of its emitted radiation. (a) Find the energy of a photon with this wavelength. J/photon(b) What is the surface temperature of the star? K(c) At what rate is energy emitted from the star in the form of radiation? Assume the star is a blackbody (e = 1). W(d) Using the answer to part (a), estimate the rate at which photons leave the surface of the star. photons/s
If it takes 10.2 eV of energy excite hydrogen from the ground state into the first excited (n = 2) state, then what frequency photon is required to excite hydrogen out of the ground state into n = 2 state? What is the wavelength (λ) of that photon? What kind of radiation (region of the electromagnetic spectrum) is this photon?
Albert Einstein is pondering how to write his (soonto-be-famous) equation. He knows that energy E is a function of mass m and the speed of light c, but he doesn't know the functional relationship (E = m2c? E = mc4?). Pretend that Albert knows nothing about dimensional analysis, but since you are taking a fluid mechanics class, you help Albert come up with his equation. Use the step-by-step method of repeating variables to generate a dimensionless relationship between these parameters, showing all of your work. Compare this to Einstein's famous equation—does dimensional analysis give you the correct form of the equation?
What is the wavelength in micrometers of peak emission for a black body at 33.5°C? (c = 3.0 × 108 m/s, Wien displacement law constant is 2.9 × 10-3 m ∙ K, σ = 5.67 × 10-8 W/m2 ∙ K4). Please give your answer with one decimal place.
Consider a model of an electron as a hollow sphere with radius R and the electron charge -e spread uniformly over that surface. d. Use Einstein’s equation relating rest mass to energy to derive a value for R. Unfortunately, your answer will be model-dependent. The traditional “Classical radius of the electron” is derived by setting the electrostatic work to be e2/(4pi e0 R)
The Schwarzschild radius of a black hole is the point at which the escape velocity equals that of light. Consider a sphere of mass M and radius R (a) Using classical physics, write down the escape velocity from the sphere’s surface. Find the value of R for which it equals the speed of light. If the mass, M, is entirely inside this radius, it is a black hole. (b) What is this radius for a star of 10 solar masses? (c) What is its average density inside this radius? (Note, the full general relativistic result happens to agree with the same formula)
Is this a maxwell-boltzman distribution curve or is this a curve having to with blackbody radiation?I think it is a boltzmann distribution.
A star’s spectrum emits more radiation with a wavelength of 690.0 nm than with any other wavelength. If the star is 9.78 ly from Earth and its radius is 7.20 × 108 m, what will an Earth-based observer measure for this star’s intensity? Stars are nearly perfect blackbodies. (Note: ly stands for light-years.) Answer in W/m2
How is Ψ(x,t) different than a classical wave? How is it similar to a classical particle?
Using Wien's Law for two black body objects with a temperature of 1000 K (fire) and 290 K (background), at what central wavelengths are the two objects radiating?
Explain the following concepts: If you observe objects inside a very hot kiln, why is it difficult to discern the shapes of the objects? Why is an electron microscope more suitable than an optical microscope for “seeing” objects of atomic size? Are blackbodies black? Why is it impossible to simultaneously measure the position and velocity of a particle with infinite accuracy? All objects radiate energy. Why, then, are we not able to see all the objects in a dark room? Is light a wave or a particle? Support your answer by citing specific experimental evidence. In the photoelectric effect, explain why the stopping potential depends on the frequency of the light but not on the intensity. provided sources using APA format.
Let the mass of the sun be denoted by Ms and its radiative power P. Determine the smallest possible spherical dust particle of density D that can stay in the solar system. Hint: compare the attractive gravitational force with the repulsive radiative force