The mathematics which govern these processes are highly non-linear differential equations, and it is gratifying that the results that these equations yield, match superbly the features of the HR diagram.Įventually, gravity will force the core of the star to contract while the outer layers of the former star will puff out into a planetary nebula. It is a highly complicated state of affairs, because stars of different masses will have different core temperatures, and hence differing abilities to burn each element in its interior. Eventually, when all its nuclear fuel is consumed, the core will lack the proper conditions to continue fusion burning. In the red giant phase and beyond, the star will start a complicated set of fusion reactions which changes the structure significantly. All of this increased radiation causes the star's envelope to expand outward into its new stage of evolution, the red giant phase. The increased temperature also triggers a shell of hydrogen to begin fusing around the star's core in the aptly named process called hydrogen shell burning. When all of the hydrogen is consumed, the gravitational force will compress the core further, raising it to a temperature high enough for it to begin fusing helium, which temporarily prevents further collapse. Low mass stars, such as our own sun, spend the majority of their lifetime (billions of years) on the main sequence where they maintain hydrostatic equilibrium by transmuting hydrogen into helium in their stellar cores through the process known as nuclear fusion. Download a PDF of the paper titled Formation of GW190521 from stellar evolution: the impact of the hydrogen-rich envelope, dredge-up and $^$O rate can lead to theįormation of BHs with masses consistent with the primary component of GW190521.Analyzing the Universe - Course Wiki: Life-Cycles of Stars A Closer Look at the Stars: Stellar Evolution
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