Conceptual question on the eddington limit

In summary, the Eddington Limit is the theoretical limit for the amount of radiation a star can emit before becoming unstable. It is calculated using an equation by Sir Arthur Eddington and plays a crucial role in the evolution of stars, leading to processes such as mass loss and nuclear fusion. While stars can temporarily exceed the Eddington Limit, they will eventually return to a stable state. There have been observed cases of stars reaching or exceeding this limit, such as Eta Carinae and other pulsating variable stars and supernovae.
  • #1
channel1
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How are magnetars self-sustaining in light of the fact that they surpass the Eddington Limit?
L_Eddington=4πcGMm/σ_T

I read that that was a big reason the sources of the superstrong g-ray bursts were originally believed to be closer than magnetars actually are but I can't find why they aren't completely having their outer layers blown off...
 
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  • #2
Is this really a homework question?
 

FAQ: Conceptual question on the eddington limit

What is the Eddington Limit and why is it important in astrophysics?

The Eddington Limit is the theoretical limit for the amount of radiation that a star can emit before the outward pressure of the radiation overcomes the inward gravitational force. It is important in astrophysics because it determines the maximum size and luminosity that a star can reach before it becomes unstable and potentially explodes.

2. How is the Eddington Limit calculated?

The Eddington Limit is calculated using the Eddington luminosity equation, which takes into account the mass and composition of the star, as well as the radiation pressure and opacity of the materials within the star. This equation was developed by British astrophysicist Sir Arthur Eddington in the early 20th century.

3. Can a star exceed the Eddington Limit?

Yes, a star can temporarily exceed the Eddington Limit if it undergoes a rapid increase in luminosity, such as during a supernova explosion. However, this is only a temporary state and the star will eventually return to a stable state below the Eddington Limit.

4. How does the Eddington Limit affect the evolution of stars?

The Eddington Limit plays a crucial role in the evolution of stars. As a star reaches its Eddington Limit, it becomes unstable and can undergo processes such as mass loss, increased nuclear fusion, or even a complete collapse. This can lead to the formation of new stars and the recycling of materials in the universe.

5. Are there any known examples of stars reaching the Eddington Limit?

Yes, there have been observed cases of stars reaching or even exceeding the Eddington Limit. One notable example is the star Eta Carinae, which is estimated to have reached 5 million times the luminosity of our Sun before undergoing a major eruption in the 19th century. Other examples include pulsating variable stars and highly luminous supernovae.

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