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The wavelength 10.0 μm is in the infrared region of the electromagnetic spectrum, whereas 600 nm is in the visible region and 100 nm is in the ultraviolet. What is the temperature of an ideal blackbody for which the peak wavelength λm is equal to each of these wavelengths?

Short Answer

Expert verified
289.8 K, 4830 K, and 28980 K for 10.0 µm, 600 nm, and 100 nm, respectively.

Step by step solution

01

Understand the Problem

We need to calculate the temperature of an ideal blackbody for which its peak wavelength λm corresponds to specific given wavelengths: 10.0 μm, 600 nm, and 100 nm. These values indicate the type of electromagnetic region based on wavelength.
02

Recall Wien's Displacement Law

Wien's Displacement Law relates the temperature T of a blackbody to its peak wavelength λm using the formula: λmT=2.898×103 m K. We will use this formula to find T for each given wavelength.
03

Convert Units for Consistency

Before substituting the wavelength values into Wien's displacement law, convert them to meters: 10.0μm=10.0×106 m,600 nm=600×109 m,100 nm=100×109 m.
04

Calculate Temperature for 10.0 µm

Using Wien's law, set λm=10.0×106 m: T=2.898×10310.0×106=289.8 K.
05

Calculate Temperature for 600 nm

With λm=600×109 m: T=2.898×103600×109=4830 K.
06

Calculate Temperature for 100 nm

For λm=100×109 m: T=2.898×103100×109=28980 K.
07

Conclusion

The corresponding temperatures are 289.8 K for 10.0 μm, 4830 K for 600 nm, and 28980 K for 100 nm.

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Key Concepts

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

blackbody radiation
Blackbody radiation refers to the electromagnetic radiation emitted by an object that absorbs all radiation incident upon it, making it a perfect absorber. This type of emitter is also known as an ideal blackbody. Such objects do not reflect or transmit any radiation and instead, hold all energy within them, emitting a continuous spectrum that depends solely on their temperature.
Understanding blackbody radiation is crucial as it serves as a fundamental model for describing how objects emit thermal radiation. The energy emitted by a blackbody is distributed across various wavelengths, and the intensity depends on the temperature of the blackbody.
Scientists use blackbody radiation concepts to understand real-world objects like stars and planets, which approximate ideal blackbody behavior by emitting radiation based on their temperature. Even though real-world objects are not perfect blackbodies, they often exhibit behavior similar enough to make these concepts very useful in astrophysics and thermal physics.
electromagnetic spectrum
The electromagnetic spectrum encompasses all types of electromagnetic radiation, ranging from very low-energy radio waves to extremely high-energy gamma rays. Light, as we see it, is just a tiny part of this expansive spectrum.
Key regions of the electromagnetic spectrum include:
  • Radio waves
  • Microwaves
  • Infrared
  • Visible light
  • Ultraviolet
  • X-rays
  • Gamma rays
Each category within the spectrum is distinguished by its wavelength range. For instance, visible light comprises colors from violet (shortest wavelength) to red (longest wavelength).
Researchers across various fields, including astronomy and medicine, utilize different parts of the electromagnetic spectrum to explore the universe and diagnose health conditions, respectively. Understanding how each region of the spectrum behaves helps scientists unlock numerous practical applications.
peak wavelength
The peak wavelength is a critical concept in understanding blackbody radiation. It refers to the specific wavelength at which the emission of radiation from a blackbody is at its maximum.
According to Wien's Displacement Law, there's an inverse relationship between the temperature of a blackbody and its peak wavelength. This means that as the temperature of a blackbody increases, the peak wavelength, where the radiation is most intense, shifts to shorter values. This principle allows us to draw conclusions about the temperature of stars and other celestial bodies, simply by determining their peak wavelengths. Wien's Displacement Law is expressed mathematically as: λmT=2.898×103 m K where λm is the peak wavelength and T is the temperature of the blackbody.
infrared
Infrared radiation is a part of the electromagnetic spectrum with wavelengths longer than visible light but shorter than radio waves. Typically, infrared wavelengths range from about 700 nm to 1 mm.
Infrared radiation is not visible to the human eye but can be felt as heat. Objects emit infrared radiation as a function of their temperature, which makes this region valuable in understanding thermal characteristics of substances.
In everyday life, infrared is commonly used in:
  • Remote controls
  • Night-vision devices
  • Thermal imaging cameras
  • Infrared heaters
This radiation also plays an essential role in meteorology, astronomy, and medicine, such as spectroscopy, enhancing the understanding of both the Earth's atmosphere and distant celestial objects.
ultraviolet
Ultraviolet (UV) radiation consists of electromagnetic waves with wavelengths shorter than visible light, typically ranging from about 10 nm to 400 nm. UV radiation falls just beyond the violet end of the visible spectrum.
UV radiation is not visible to the naked eye, but it carries enough energy to cause chemical reactions, which makes it both useful and dangerous. For example, UV rays are crucial for synthesizing vitamin D in the skin, yet overexposure can result in skin damage and increase cancer risk.
Key uses of ultraviolet radiation include:
  • Sterilization and disinfection
  • Fluorescence studies in laboratory settings
  • Water purification
  • Studying the composition of stars and galaxies in astronomy
Understanding UV radiation helps scientists address health issues related to sun exposure and enhances our knowledge about interstellar matter.

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Most popular questions from this chapter

Why is it easier to use helium ions rather than neutral helium atoms in such a microscope? (a) Helium atoms are not electrically charged, and only electrically charged particles have wave properties. (b) Helium atoms form molecules, which are too large to have wave properties. (c) Neutral helium atoms are more difficult to focus with electric and magnetic fields. (d) Helium atoms have much larger mass than helium ions do and thus are more difficult to accelerate.

What must be the temperature of an ideal blackbody so that photons of its radiated light having the peak-intensity wavelength can excite the electron in the Bohr-model hydrogen atom from the ground level to the n = 4 energy level?

(a) What accelerating potential is needed to produce electrons of wavelength 5.00 nm? (b) What would be the energy of photons having the same wavelength as these electrons? (c) What would be the wavelength of photons having the same energy as the electrons in part (a)?

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.

(a) Using the Bohr model, calculate the speed of the electron in a hydrogen atom in the n = 1, 2, and 3 levels. (b) Calculate the orbital period in each of these levels. (c) The average lifetime of the first excited level of a hydrogen atom is 1.0 × 108 s. In the Bohr model, how many orbits does an electron in the n = 2 level complete before returning to the ground level?

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