Fraunhofer Lines: Absorption & Re-emission in Solar Atmosphere

In summary: This is because the frequencies are being blocked by the atmosphere. In summary, the Fraunhoffer lines are dark because the frequencies are being blocked by the atmosphere.
  • #1
Anton Alice
68
1
Hello people,

I was wondering, why the absence of certain frequencies in the sun spectrum (fraunhofer lines) is so strong? In all pictures I have seen so far these lines are very dark, so there is nothing reaching us at these frequencies. Why is that?

The absorption occurs in the solar atmosphere. But also, there must be a re-emission of these missing frequencies, and the re-emission occurs in all spatial directions equally. Therefore some of the light should be able to exit the solar atmosphere, because the probability of going back to the sun equals the probability of going the other way around.
 
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  • #2
Anton Alice said:
Hello people,

I was wondering, why the absence of certain frequencies in the sun spectrum (fraunhofer lines) is so strong? In all pictures I have seen so far these lines are very dark, so there is nothing reaching us at these frequencies. Why is that?

The absorption occurs in the solar atmosphere. But also, there must be a re-emission of these missing frequencies, and the re-emission occurs in all spatial directions equally. Therefore some of the light should be able to exit the solar atmosphere, because the probability of going back to the sun equals the probability of going the other way around.
The Fraunhoffer lines occur when light passes through relatively cool gas surrounding the Sun. The gas is too cool to radiate those frequencies. You can see the same in the lab if you pass a sodium light through a flame into which a bit of salt has been placed. The Fraunhoffer lines are best seen when the light beam passes through the cool area above the incandescent flame.
 
  • #3
The temperature in the solar atmosphere is about 6000K, why is this low? Do you mean, that there are only few collisions occurring?
tech99 said:
The gas is too cool to radiate those frequencies.
But at some point in time the gas in the solar should be saturated with exited atoms, and all the light should be able to pass through.

The exited state in a single, isolated Atom (no collisions) should still have an intrinsic and finite lifetime due to vacuum fluctuation.
 
  • #4
Anton Alice said:
these lines are very dark, so there is nothing reaching us at these frequencies.

They only appear (to our eyes+brain) to be very dark, by contrast with the adjacent bright sections of the spectrum.
 

What are Fraunhofer lines?

Fraunhofer lines are dark lines in the solar spectrum that correspond to specific wavelengths of light that have been absorbed by elements in the solar atmosphere.

Why are Fraunhofer lines important?

Fraunhofer lines are important because they provide information about the chemical composition and temperature of the solar atmosphere. By analyzing these lines, scientists can identify the elements present in the Sun and study its physical properties.

How are Fraunhofer lines formed?

Fraunhofer lines are formed when light from the Sun's surface passes through its atmosphere. Elements in the atmosphere absorb specific wavelengths of light, leaving dark lines in the spectrum. These lines are then observed and analyzed by scientists.

What is the significance of absorption and re-emission in Fraunhofer lines?

The absorption and re-emission process in Fraunhofer lines is important because it allows scientists to study the physical conditions of the solar atmosphere. The absorbed light is re-emitted in all directions, providing information about the temperature and density of the absorbing elements.

Can Fraunhofer lines be observed from Earth?

Yes, Fraunhofer lines can be observed from Earth using a spectroscope. By splitting the light from the Sun into its component wavelengths, scientists can identify and study the dark lines in the spectrum, providing valuable insights into the composition and properties of the Sun.

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