The standard solar model
The Sun is the most prominent object in our sky, and understanding it has been one of the primary focuses since the birth of modern astronomy. Additionally, after the realization that the Sun was itself a star, solar research became a means for investigating conditions too distant to observe directly. Starting in the early twentieth century, astronomers began building a model of the Sun that would accurately predict the Sun¡¯s observable features. If the model can accurately predict what is observed, then it is reasonable to assume that it can accurately tell astronomers about what they cannot observe, both inside the Sun and its behavior at other epochs. This model is known as the standard solar model, and it has been in a state of constant evolution since its inception. The standard solar model has four basic assumptions;1. The first being that the sun evolves in hydrostatic equilibrium. 2. The second assumption of the standard solar model is that energy can be transferred in the star via radiation, conduction, convection, and neutrino losses. 3. The third assumption of the model is that thermonuclear reactions are the only source of energy production inside the star.
Some topics in this essay:
HYDROSTATIC EQUILIBRIUM, THERMONUCLEAR REACTIONS, Specifically CNO, PPIII Absorbing, Conduction Conduction, INTRODUCTION Sun, PPI PPII, PPII Chains, Conclusions Overall, Transport Photons, e+ +, solar model, + ¦Í, + 1h, standard solar model, standard solar, e+ + ¦Í, hydrostatic equilibrium, hydrogen nuclei, + e+, + ¦Ã, pp chain, + e+ +, + 1h ¡ú, method energy transport,
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Approximate Word count = 2570
Approximate Pages = 10 (250 words per page double spaced)
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