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The shortest visible wavelength is about 400 nm. What is the temperature of an ideal radiator whose spectral emittance peaks at this wavelength?

Short Answer

Expert verified
The temperature is approximately 7242.5 K.

Step by step solution

01

Apply Wien's Displacement Law

Wien's Displacement Law relates the peak emission wavelength (\( \lambda_{max} \)) of a blackbody to its temperature (\( T \)). The law is given by:\[\lambda_{max} T = b\]where \( b \) is Wien's displacement constant, approximately \( 2.897 \times 10^{-3} \) m K.
02

Convert Wavelength to Meters

First, convert the given wavelength from nanometers to meters. Since 1 nm = \( 10^{-9} \) m:\[ 400 \text{ nm} = 400 \times 10^{-9} \text{ m} = 4.0 \times 10^{-7} \text{ m} \]
03

Solve for Temperature

Use Wien’s Displacement Law to solve for the temperature \( T \):\[T = \frac{b}{\lambda_{max}}\]Substituting \( b = 2.897 \times 10^{-3} \) m K and \( \lambda_{max} = 4.0 \times 10^{-7} \text{ m} \):\[T = \frac{2.897 \times 10^{-3}}{4.0 \times 10^{-7}} \approx 7242.5 \text{ K}\]
04

Validate Units and Calculation

Ensure that the units cancel correctly to give temperature in Kelvin and verify the calculation:The units for \( b \) are m K, and for wavelength \( \lambda_{max} \), they are meters. Thus, \( m/m \) leaves Kelvin:\[ T = \frac{2.897 \times 10^{-3} \, \text{m K}}{4.0 \times 10^{-7} \, \text{m}} = 7242.5 \, \text{K}\]The calculation confirms that the ideal radiator's temperature is approximately 7242.5 K.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Spectral Emittance
Spectral emittance refers to the energy radiated by a blackbody per unit area, per unit time, and per unit wavelength. It is a measure of how much energy is emitted at a specific wavelength. The concept helps us understand which wavelengths carry the most energy and how the emission is distributed across different wavelengths.

In the context of blackbody radiation, spectral emittance essentially tells us how strong the emission is at each part of the spectrum. Each object can emit energy over a range of wavelengths, but the intensity varies with each one. The sun, for example, emits most of its energy in the visible light spectrum, which is why it appears bright to us during the daytime.

Understanding spectral emittance is vital in fields like astronomy and climate science. It helps scientists predict how an object will look at different temperatures and what its spectral signature might be. This information is crucial when looking at stars or planets and trying to understand their temperature and composition without physically being there.
  • Measured in watts per square meter per nanometer (W m⁻² nm⁻¹).
  • Determines how colors appear in photography or display technology.
  • Important for estimating energy output of stars and planets.
Blackbody Radiation
Blackbody radiation is the emission of electromagnetic radiation by an idealized object that absorbs all incoming light, known as a "blackbody". It is characterized by a spectrum of wavelengths that only depends on the temperature of the body, not on its material or structure.

A perfect blackbody doesn't reflect or transmit any light; it only emits radiation. This radiation is in equilibrium with any corresponding absorption due to the object’s temperature. The spectrum of blackbody radiation is continuous and covers a wide range of wavelengths, with a distinct peak at a wavelength that depends on temperature. This is where Wien's Displacement Law is handy, as it articulates that the peak wavelength shifts with changes in temperature.

The sun is a great example of a blackbody, as it emits radiation over a wide range of wavelengths. By studying the blackbody radiation emitted, we can infer many properties about celestial objects, including temperature.
  • Characterized by its Planck's Law spectrum.
  • Temperature affects peak emission wavelength.
  • Helps scientists model heat emission from stars and planets.
Peak Emission Wavelength
The peak emission wavelength is the specific wavelength at which a blackbody's emission is maximized. In simple terms, it is the color or type of light that a body at a particular temperature emits most intensely. This peak shifts with temperature changes and is critical in understanding blackbody radiation's characteristics.

Wien's Displacement Law directly relates temperature to peak emission wavelength, as detailed in the solution above. Higher temperatures result in shorter peak wavelengths - meaning hotter objects tend to be bluer, because blue light has a shorter wavelength. Conversely, cooler objects peak at longer wavelengths and appear redder.

This concept is not only central to astronomy and physics but is also widely used in applications like thermal imaging and material sciences. Knowing the peak emission wavelength allows scientists to estimate the temperature of distant stars by simply analyzing the light they emit.
  • Moves to shorter wavelengths as temperature increases.
  • Provides an indication of an object's surface temperature.
  • Enables the study and comparison of stars and heated objects.

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Most popular questions from this chapter

(a) A particle with mass \(m\) has kinetic energy equal to three times its rest energy. What is the de Broglie wavelength of this particle? (\(Hint\): You must use the relativistic expressions for momentum and kinetic energy: \(E^2 = (pc^2) + (mc^2)^2\) and \(K = E - mc^2\).) (b) Determine the numerical value of the kinetic energy (in MeV) and the wavelength (in meters) if the particle in part (a) is (i) an electron and (ii) a proton.

For your work in a mass spectrometry lab, you are investigating the absorption spectrum of one-electron ions. To maintain the atoms in an ionized state, you hold them at low density in an ion trap, a device that uses a configuration of electric fields to confine ions. The majority of the ions are in their ground state, so that is the initial state for the absorption transitions that you observe. (a) If the longest wavelength that you observe in the absorption spectrum is 13.56 nm, what is the atomic number Z for the ions? (b) What is the next shorter wavelength that the ions will absorb? (c) When one of the ions absorbs a photon of wavelength 6.78 nm, a free electron is produced. What is the kinetic energy (in electron volts) of the electron?

Suppose that the uncertainty of position of an electron is equal to the radius of the \(n\) = 1 Bohr orbit for hydrogen. Calculate the simultaneous minimum uncertainty of the corresponding momentum component, and compare this with the magnitude of the momentum of the electron in the \(n\) = 1 Bohr orbit. Discuss your results.

If your wavelength were 1.0 m, you would undergo considerable diffraction in moving through a doorway. (a) What must your speed be for you to have this wavelength? (Assume that your mass is 60.0 kg.) (b) At the speed calculated in part (a), how many years would it take you to move 0.80 m (one step)? Will you notice diffraction effects as you walk through doorways?

How does the wavelength of a helium ion compare to that of an electron accelerated through the same potential difference? (a) The helium ion has a longer wavelength, because it has greater mass. (b) The helium ion has a shorter wavelength, because it has greater mass. (c) The wavelengths are the same, because the kinetic energy is the same. (d) The wavelengths are the same, because the electric charge is the same.

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