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Stellar Physics and Evolution

This overview explores the fascinating processes of stellar evolution, focusing on the gravitational pressures and nuclear fusion mechanisms within a star's core. It details how hydrogen is fused into helium through hydrostatic equilibrium and the role of gravitational forces in maintaining stability. As hydrogen depletes, helium fusion begins, prompting expansion into a red giant phase. Understanding these transformations is key to grasping the lifecycle of main sequence stars and their eventual fate in the universe.

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Stellar Physics and Evolution

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  1. Stellar Physics and Evolution

  2. Gravitation Pressure

  3. Gravitation Pressure

  4. Gravitation Pressure Fusion Core 4H 4He + hf

  5. Gravitation Pressure Fusion Core

  6. Gravitation Pressure Fusion Core Hydrostatic Equil Gravitation = radiation Main Sequence Star Hydrogen fusion

  7. Hydrogen Gone

  8. Core Contracts

  9. Helium fusion Begins

  10. Envelope expands to Red Giant

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