After the hydrogen in the core of a star is used up the star moves off the main-sequence, and as the core becomes denser and hotter other fusions could happen. When the core mass density is on the order of 106 kg m−3, at what temperature would electron degeneracy pressure become important in the core? For the electron degeneracy pressure to be more important, should the temperature increase or decrease?
After the hydrogen in the core of a star is used up the star moves off the main-sequence, and as the core becomes denser and hotter other fusions could happen. When the core mass density is on the order of 106 kg m−3, at what temperature would electron degeneracy pressure become important in the core? For the electron degeneracy pressure to be more important, should the temperature increase or decrease?
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After the hydrogen in the core of a star is used up the star moves off the main-sequence, and as the core becomes denser and hotter other fusions could happen. When the core mass density is on the order of 106 kg m−3, at what temperature would electron degeneracy pressure become important in the core? For the electron degeneracy pressure to be more important, should the temperature increase or decrease?
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