Lecture 4 - Astro Pas Rochester

More documents

Recommendations

Info

The equations of stellar structure (continued) ! There are no general, analytical solutions to the equations; usually stellar-interior models are generated by computer solution. ! Instead of solving these equations, we shall employ some crude approximations to develop several scaling relationships that will also be crude, but will correctly illuminate the physical processes important in stars. ! First we will derive the equation of hydrostatic equilibrium. <strong>Astro</strong>nomy 142 6
Hydrostatic equilibrium Consider a spherical shell of radius r and thickness Δr
Page 1 and 2: Today in Astronomy 142: stellar str
Page 3 and 4: Principles of stellar structure (co
Page 5: These equations can be derived from
Page 9 and 10: Another way to derive this, using E
Page 11 and 12: The Sun’s interior, on the averag
Page 13 and 14: Central pressure in a star (continu
Page 15 and 16: For the Sun: Central pressure in a
Page 17 and 18: Central density and temperature of
Page 19 and 20: Diffusion of energy to the surface
Page 21 and 22: Opacity and luminosity in stars (co
Page 23 and 24: Diffusive approximations @f(x, t) @
Page 25: Summary ! Using hydrostatic equilib

Lecture 4 - Astro Pas Rochester

Create successful ePaper yourself

Delete template?

Save as template?