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The Sun's Evolution: Past, Present, and Future

Explore the methods, values of M, R, L, and t, opacities, presolar helium, and mixing length influencing the Sun's evolution. Delve into mass loss, convection, and the Sun's radial excursions in the HR diagram.

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The Sun's Evolution: Past, Present, and Future

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  1. Our Sun. III. Present and Future(1993ApJ_418_475s) Jae Gyu, Byeon

  2. Contents • Methods • Values of M, R, L, and t • Opacities • Presolar Helium and the Mixing Length • Mass Loss • Results • The Sun’s evolution in the HR diagram • The Sun’s Mass Loss • Convection • The Sun’s Radial Excursions • Conclusions

  3. Methods • Values of M⊙, R⊙, L⊙, and t⊙ • The solar mass is M⊙ = 1.9891 × 1033 g • The solar radius at an optical depth of 0.001 is R⊙ = 6.9598 × 1033 cm • The Solar luminosity L⊙ = 3.854 × 1033 erg s-1 • T⊙ = 4.55 Gyr • Opacities • Use the Los Alamos Opacity from Keady(1985) • At low temperatures, use the molecular opacities by Keady • Modify recent molecular opacities of Sharp(1992)

  4. Methods • Presolar Helium and the Mixing Length • Presolar helium abundance, Y = 0.274 • Mixing Length parameter, α = 2.10 • Metallicity Z = 0.01954 • Mass Loss • η is the mass-loss parameter • Normalized from the RGB mass loss inferred from (low mass) globular cluster horizontal branch stars • Solar mass loss of 0.275 M⊙ on the RGB and 0.184 M⊙on the AGB

  5. The Sun’s evolution in the HRD

  6. The Sun’s evolution in the HRD

  7. The Sun’s Mass Loss

  8. Convection

  9. The Sun’s Radial Excursions

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