Blackbody effect hypothetical question

In summary, according to the blackbody effect, objects can become so hot that they emit no visible light. However, the spectrum of the emitted radiation still includes all wavelengths, just with a peak in the ultraviolet or even x-ray range. This is because as the temperature increases, the energy emitted in all wavelength bands increases. This means that even as more energy is emitted in the UV or x-ray range, there is still an increase in the amount of visible light emitted. This is also demonstrated by the fact that there are blue stars, which are objects that are extremely hot and emit mostly blue light.
  • #1
Badmouton
7
0
According to the blackbody effect, can something be so hot that it emits no visible light?
I say this because the more heated an object is, the more it moves away from the visible light spectrum, does that apply until there is no light at all?
 
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  • #2
Not really. The spectrum of the emitted radiation includes all wavelengths. What happens is that the peak moves to ultraviolet or even x-rays, but it is still visible.
 
  • #3
As you heat a body, the energy it emits in any particular wavelength band strictly increases, so even though you are proportionally increasing the amount emitted in UV or x-ray, you are still increasing the amount in the visual spectrum.
 
  • #4
Nabeshin said:
As you heat a body, the energy it emits in any particular wavelength band strictly increases, so even though you are proportionally increasing the amount emitted in UV or x-ray, you are still increasing the amount in the visual spectrum.

As demonstrated here:-

F18-02%20Planck%20black%20body.jpg


I would like to know if it ever gets 'blue hot'.

Google says yes - blue stars.

http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html
 
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  • #5


Yes, it is possible for an object to become so hot that it emits no visible light. This phenomenon is known as a blackbody radiator, where the object absorbs and emits all radiation that falls on it. As the temperature of the object increases, the peak of its emission spectrum shifts towards shorter wavelengths, eventually reaching the ultraviolet and then the X-ray region. At extremely high temperatures, the object's emission spectrum may not include any visible light, making it appear black to our eyes. This is due to the fact that at these high temperatures, the object's atoms are excited to such a level that they emit most of their energy in the form of non-visible radiation. However, it is important to note that even at these extreme temperatures, the object will still emit some amount of visible light, just not enough for us to see it.
 

Related to Blackbody effect hypothetical question

1. What is the blackbody effect?

The blackbody effect is a hypothetical concept in physics that describes an ideal object that absorbs all electromagnetic radiation that falls on it, without reflecting or transmitting any of it.

2. Why is the blackbody effect important?

The blackbody effect is important because it helps us understand the behavior of real objects that absorb and emit radiation, such as stars and planets. It also serves as a useful theoretical model for studying thermodynamics and quantum mechanics.

3. How does the blackbody effect relate to temperature?

The blackbody effect is directly related to temperature, as the amount and frequency of radiation emitted by a blackbody is determined by its temperature. As the temperature of a blackbody increases, the amount of radiation it emits also increases, and the peak wavelength of the radiation shifts towards shorter wavelengths.

4. Can the blackbody effect be observed in real objects?

While the ideal blackbody does not exist in nature, many real objects, such as stars and planets, closely approximate the behavior of a blackbody. This is known as blackbody radiation and can be observed and measured in the form of infrared, visible, and ultraviolet light.

5. How is the blackbody effect calculated?

The blackbody effect can be calculated using Planck's law, which describes the relationship between the temperature and the amount and frequency of radiation emitted by a blackbody. It can also be approximated using the Stefan-Boltzmann law, which relates the total radiation emitted by a blackbody to its temperature.

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