Stars in the early universe and stellar processes

AI Thread Summary
The discussion centers on the formation of stars in the early universe, particularly regarding the CNO cycle and the necessity of prior stellar generations for carbon production. It is established that first-generation stars primarily composed of hydrogen and helium could not initiate the CNO cycle due to a lack of heavier elements. However, sufficiently massive stars can generate carbon through the triple-alpha process, enabling a transition to CNO dominance relatively quickly. The conversation also touches on the implications of density fluctuations in primordial gas clouds for star formation and the potential for black hole creation from short-lived massive stars. Overall, the dialogue emphasizes the complex interplay of stellar evolution, nucleosynthesis, and the conditions necessary for the emergence of different stellar types in the early universe.
  • #51
What does a star passing through Hayashi forbidden zone look like?
There are 2 ways for a star to exist in Hayashi forbidden zone: either it is hydrostatically supported by degeneracy pressure, in which case it is small and of low luminosity, or else it is rapidly contracting.
And a star contracting through Hayashi forbidden zone should be big and bright (in near-infrared).
Since a lot of brown dwarfs are seen in near-IR, despite being small and dim, how about big and bright protostars in Hayashi forbidden zone?
 
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  • #52
snorkack said:
What does a star passing through Hayashi forbidden zone look like?
It isn't called a star at all, that's star formation. And as I said, one needs a different approach to answer that question-- rather than the approach we take for stars, which is asking "what set of simplifiying idealizations can help us understand the basic structure of stars in such a way that time becomes a kind of external driving parameter", one needs to follow the time evolution explicitly from stage to stage. That is much more difficult, because you cannot know what is happening in any stage without first knowing the situation in the previous stage.
There are 2 ways for a star to exist in Hayashi forbidden zone: either it is hydrostatically supported by degeneracy pressure, in which case it is small and of low luminosity, or else it is rapidly contracting.
As I said above, the Hayashi limit does not apply for degeneracy, it applies for ideal gases. Including degeneracy allows a continuous transition from star models to brown dwarf models to planet models, all the way down to the blueprints for your house. But the topic of the thread was defined early on.
Since a lot of brown dwarfs are seen in near-IR, despite being small and dim, how about big and bright protostars in Hayashi forbidden zone?
As I said, brown dwarfs can have long-lived phases in that region, because they can be in a stable hydrostatic equilibrium. Stars like the Sun, which are not degenerate until they become white dwarfs, cannot.
 
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