At which time did the CMB become dark?

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In summary, the Cosmic Microwave Background (CMB) was emitted as a glowing yellowish-white radiation at 3000 K and as space expanded, it became redder and eventually fell into non-visible infrared. There is no specific age at which the CMB background turned from red to infrared, but it got darker over time. The present temperature of the CMB is 2.7 K and it became visible at around 800 K, which corresponds to z=300 or 3 million years after the Big Bang. Further discussion on the behavior of photons in plasma and the recombination of hydrogen can be found in the provided links.
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Gerinski
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At the time the CMB was emitted it was a glowing yellowish-white radiation at 3000 K. From there as space expanded it became redder and redder eventually falling into what for humans is non-visible infrared.
At which age of the universe did the CMB background turn from red to infrared?
Thanks
 
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To estimate this, you need to know:
-the dependence of the temperature ##T## of the CMB with time/scale factor ##a## of the universe, which is roughly ##T \propto \frac{1}{a}##
-the evolution of the scale factor with time, from the Friedman equation which gives for a matter-dominated universe ##\frac{a}{a_0}=(\frac{t}{t_0})^{2/3}##
Then you can get the ##t## you look for by choosing the temperature you want in the following equation: ##t = t_0(\frac{T_0}{T})^{3/2}## where ##t_0## would be present time (13.8 billion years) and ##T_0## would be the present temperature of the CMB, 2.73 Kelvin degrees.
 
  • #3
There is no hard threshold, it just got darker over time. Based on those arbitrary categories, thermal radiation becomes visible somewhere around 525°C, or ~800 K. Today the temperature is 2.7 K, so we are talking about z=300. Based on this cosmology calculator, this was around 3 million years after the Big Bang.

"Cherry red" at 1000 K corresponds to z=370, 2.2 million years after the Big Bang.
 
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Thanks a lot.
 
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Chronos said:
Photons do not play well in plasma, largely due to a phenomenon known as Compton scattering. This same effect makes it difficult to see anything below the atmosphere of a star. For futher discussion, see; https://ned.ipac.caltech.edu/level5/Sept05/Gawiser2/Gawiser1.html, ORIGIN OF THE COSMIC BACKGROUND RADIATION.
Everything discussed in this thread happened after the plasma recombined enough to make scattering negligible. That is the whole point of the CMB. The hydrogen got re-ionized much later (>100 million years), but at that time it was so spread out that it didn't make the universe opaque any more.
 
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Moderator's note: some off topic posts have been removed.
 

Related to At which time did the CMB become dark?

1. What is the CMB?

The CMB (cosmic microwave background) is a faint radiation that fills the entire universe and is the oldest light in existence. It is a remnant of the Big Bang and is the most direct evidence of the universe's early state.

2. When did the CMB become dark?

The CMB did not become dark at any specific time. It has always existed since the Big Bang, but it has cooled and stretched over time, resulting in its current state as a faint microwave radiation.

3. How was the CMB discovered?

The CMB was first discovered in 1964 by American physicists Arno Penzias and Robert Wilson. They were analyzing radio waves from space when they discovered a stubborn background noise coming from all directions. After ruling out all possible sources, they realized it was the CMB.

4. What does the darkness of the CMB tell us about the universe?

The darkness of the CMB tells us that the universe is expanding and cooling. The fact that the CMB is a faint microwave radiation and not a bright light indicates that the universe has been expanding and cooling for billions of years since the Big Bang.

5. Can we see the CMB with the naked eye?

No, the CMB is not visible to the naked eye. It is a form of radiation that is invisible to human eyes. However, it can be detected by specialized instruments, such as radio telescopes, and is an important tool for studying the early universe.

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