When is a star considered a white dwarf?
When hydrogen burning is almost over the star first become red giant.
The majority of stars experience this under the Chandra-Sekhar limit, wherein no fusion occurs and the star is supported by electron degeneracy pressure. The outer layers puff out to form a planetary nebula, and the inner mass shrinks and stops with a pressure known as degenerative pressure.
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When a star runs out of nuclear fuel and collapses due to its own gravity, it becomes a white dwarf. It becomes extremely hot and dense, but it is no longer experiencing nuclear fusion reactions in its core.
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When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.
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